164 Sentences With "bright giant" | Random Sentence Generator

The primary component, HR 2554 A, is a yellow G-type bright giant with a mean apparent magnitude of +4.4.

HD 143183 lies approximately 1' from the 10th-magnitude O-class bright giant CD-53 6363, the second-brightest star in the cluster.

V337 Carinae (V337 Car, q Carinae) is a K-type bright giant star in the constellation of Carina. It is an irregular variable and has an apparent visual magnitude which varies between 3.36 and 3.44. V337 has a spectral class of K2.5II, indicating a bright giant. It is considered likely to be on the red giant branch of stars fusing hydrogen around an inert helium core.

HD 167818 is a class K3II (orange bright giant) star in the constellation Sagittarius. Its apparent magnitude is 4.66 and it is approximately 760 light years away based on parallax.

HD 20468 is a class K2II (orange bright giant) star in the constellation Perseus. Its apparent magnitude is 4.82 and it is approximately 1180 light years away based on parallax.

HD 61772 is a class K3II (orange bright giant) star in the constellation Puppis. Its apparent magnitude is 4.98 and it is approximately 700 light years away based on parallax.

HD 157662 is a bright giant star in the southern constellation of Ara. It has a magnitude 10.91 companion at an angular separation of 76.4″ along a position angle of 159°.

The brightest hot stars in the cluster have a spectral type of BC2, indicating B2 stars with enhanced levels of carbon. One has a bright giant luminosity class of II, while the other has a luminosity class of Ib-II, indicating it is either a bright giant or supergiant. The hotter stars of the cluster are visually faint due to around six magnitudes of interstellar extinction. The lack of blue supergiants, particularly in a cluster of just the right size and age to include five red supergiants, is unusual.

HD 33203 is double star in the northern constellation of Auriga. It includes a bright giant star with a stellar classification of B2II. The two components have an angular separation of 1.617″ along a position angle of 222.1°.

The binary system consists of a bright giant orbited by a dwarf companion once every four millennia or so. Compared to the Sun, Beta Draconis A is an enormous star with six times the mass and roughly 40 times the radius. At this size, it is emitting about 950 times the luminosity of the Sun from its outer envelope at an effective temperature of 5,160 K, giving it the yellow hue of a G-type star. The spectrum matches a stellar classification of G2 II, with the luminosity class of II indicating it is a bright giant.

Bright giants are stars of luminosity class II in the Yerkes spectral classification. These are stars which straddle the boundary between ordinary giants and supergiants, based on the appearance of their spectra. The bright giant luminosity class was first defined in 1943.

It is a bright giant with a nominal stellar classification of F8 II, that pulsates between spectral types F6II-G2. The star has 2.8 times the mass of the Sun and 39.2 times the Sun's radius. It is losing mass at the estimated rate of .

The star is moving closer with a heliocentric radial velocity of −28 km/s. It is a candidate runaway star showing a transverse peculiar velocity of 213.87 km/s. Houk and Smith-Moore (1978) gave this star a stellar classification of B8 II, matching a B-type bright giant.

This is an evolved bright giant with a spectral type of K0 II. It is about two times more massive and over twelve times wider than the Sun. The star is radiating 135 times the Sun's luminosity from its photosphere at an effective temperature of about 4,700 K.

HD 156768 is a double star in the southern constellation of Ara. The brighter component is a sixth magnitude bright giant or supergiant star with a stellar classification of G8Ib/II. The magnitude 9.6 companion lies at an angular separation of 1.81″ along a position angle of 184°.

M Puppis (M Pup, HR 2789, HD 57197) is a blue giant or bright giant star (spectral type B8II/III) in the constellation Puppis. Its apparent magnitude is 5.84, which means it is visible with the naked eye under optimal conditions. It is approximately 590 light years away based on parallax.

The C-N spectral type is to distinguish those stars from the C-R type where the blue continuum is not entirely hidden by absorption bands. A classification based on the infrared spectrum is C5 II, again a moderately cool carbon star with a luminosity class of II for a bright giant.

HD 64440, also known as a Puppis, is a spectroscopic binary star in the constellation Puppis. Its apparent magnitude is 3.71. Located around distant, the primary is a bright giant of spectral type K1.5II and the secondary is an early A-type star. They orbit with a period just under 7 years and eccentricity 0.38.

This object has a stellar classification of A0II, matching a massive bright giant. In the past it had received a class of B9III, which is sometimes still used. The star is 37 million years old with 7.9 times the mass of the Sun. It is spinning with a projected rotational velocity of 47 km/s.

It is a candidate member of the Volans-Carina Association of co-moving stars. The visible component is an aging bright giant star with a stellar classification of B8/9II. The spectrum of the star displays metallic lines of magnesium. The Volans-Carina Association to which it belongs has an age of 90 million years.

X Sagittarii is a bright giant Cepheid variable star in the constellation Sagittarius. This variable star changes in apparent magnitude from 4.90 to 4.20 magnitude with a period of 7.01 days. Its change in brightness is accompanied by a change in spectral classification, from G2 to F5. It is approximately 990 light years away based on parallax.

Perkins et al. (1989) found a stellar classification of for this star, suggesting it is a K-type giant with abundance anomaly of barium. Houk and Swift (1999) matched an ordinary giant with a class of K3 III. Many sources still use the 1991 Bright Star Catalogue classification of K5 II, which instead suggests a bright giant star.

LY Aurigae is a close visual binary. The two stars are magnitude 6.85 and magnitude 8.35 0.6 arc-seconds apart. Each star is also a spectroscopic binary. LY Aur A is a double-lined spectroscopic binary with an O9 bright giant and an O9 giant star in contact and eclipsing each other as they orbit every 4 days.

The luminosity class as determined from different spectral features varies from bright giant (II) to bright supergiant (Ia), with a compromise being given as M5eIbp. Early attempts at classification were confused by the interpretation of surrounding nebulosity as companion stars. The derived spectral class varies depending on the features examined. The spectral features also vary noticeably over time.

It has an absolute magnitude of −2.3. The primary is an orange-hued K5II-type star (K-type bright giant) and the secondary is a smaller blue star similar to Regulus; its period is 972 days. The secondary is a B7V-type star, a B-type main-sequence star. Zeta Aurigae's maximum magnitude is 3.7 and its minimum magnitude is 4.0.

The primary, component A, is a yellow-white hued bright giant with a stellar classification of F8 II, and it is a classical Cepheid variable. The combined apparent magnitude of the system ranges from 5.69 to 6.19 over 5.273 days. The secondary companion, component B, is a main sequence star with a class of B6 V and an absolute magnitude of about −0.12.

The variable velocity of this system was reported by W. W. Campbell in 1918. It is a single-lined spectroscopic binary with an orbital period of and an eccentricity of 0.4. The components have a visual magnitude difference of 2.7 and are unresolved by speckle interferometry. The primary component is an evolved bright giant star with a stellar classification of G5II.

The roman numerals indicate a luminosity class of bright giant. Most such stars are found in binary star systems, but this appears to be an exception as no companion has been discovered. Evolved stars with Am-like peculiarities of abundance have come to be known as ρ Puppis stars. The star's metallicity is more than double that in the Sun.

This is an evolved bright giant star with a stellar classification K2II, between the classifications of giant and supergiant. Having exhausted the supply of hydrogen at its core, it has expanded to around 33.5 times the radius of the Sun. The star is radiating 469 times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 4,642 K.

It has a peculiar velocity of and may be a runaway star. The star is a member of the BH 99 cluster. The magnitude 4.85 primary, component A, is a massive K-type supergiant or bright giant with a stellar classification of K4.5Ib-II. Houk (1978) instead listed it with a class of K4/5III: but with some uncertainty about the classification.

Nu¹ Sagittarii A is a spectral type K1 bright giant which has an apparent magnitude of +4.86. It is a microvariable with a frequency of 0.43398 cycles per day and an amplitude of 0.0078 magnitude. In 1982 it was found to have a hotter companion, Nu¹ Sagittarii B, a rapidly rotating B9 type star. The pair orbit with a period of around 370 days.

The primary component is a G-type bright giant. It is over five times as massive as the Sun, and over 77 times as wide. Its companion is a B-type main-sequence star, 3.4 times as massive as the Sun. The stars have an orbit that are oriented in such a way that they periodically eclipse each other, blocking the other star's light.

The cool component is a G2 bright giant or supergiant and is visually brighter than the hot component, so it is treated as the primary. The hot component is a late B or A type star, presumed to be a main sequence star. The observed spectrum of the primary star is G2 Ib, a yellow supergiant. It is calculated to have an absolute magnitude of −2.1.

The star is drifting further away with a radial velocity of +9 km/s. This is an aging bright giant or supergiant star that has been assigned stellar classifications of F2II and F0Ib, respectively. It has seven times the mass of the Sun and has expanded to 45 times the Sun's radius. It is spinning with a projected rotational velocity of 22 km/s.

This is a massive B-type lower-luminosity supergiant or bright giant star with a stellar classification of B1 Ib or B0.5 II, respectively. It is around 22.5 million years old with a high rate of spin, showing a projected rotational velocity of 140 km/s. J. D. Rosendhal (1973) identified weak emission features associated with an asymmetric H-alpha absorption line, providing evidence of mass loss.

Beta Pyxidis (Beta Pyx, β Pyxidis, β Pyx) is a double star located in the southern constellation Pyxis. It has an apparent visual magnitude of 3.954, making it the second brightest star in that faint constellation. Based upon parallax measurements, the star is an estimated 420 light-years (128 parsecs) from the Earth. The spectrum matches a bright giant or supergiant star of stellar classification G7Ib-II.

The Bright Star Catalogue lists this star with a stellar classification of G2.5 IIa, indicating it is an evolved G-type bright giant. Gray et al. (2001) gave it a class of G1 II, while Keenan and McNeil (1989) assigned this star to the giant class G2.5 IIIa. It has an estimated 3.72 times the mass of the Sun and about 31 times the Sun's radius.

This is a B-type bright giant star with a stellar classification of B8 II. It is a Mercury-Manganese star, showing an overabundance of these elements in its spectrum. The mean longitudinal magnetic field strength is . The star has about four times the mass of the Sun and is radiating 490 times the Sun's luminosity from its photosphere at an effective temperature of 13,500 K.

HR 2554, also known as V415 Carinae and A Carinae, is an eclipsing spectroscopic binary of the Algol type in the constellation of Carina whose apparent visual magnitude varies by 0.06 magnitudes and is approximately 4.39 at maximum brightness. Its primary is a G-type bright giant star and its secondary is an A-type main sequence star. It is approximately 553 light years from Earth.

The secondary is nearly three magnitudes fainter than the primary at magnitude 7.5, and is hotter than the primary with a spectral type of B9.5. Nu Herculis's spectral type of F2 II means that it is an F-type bright giant, with a luminosity 799 times that of the Sun. Its effective temperature is 6,410 K, hotter than the Sun. Its mass is about 5.3 solar masses.

This is a probable astrometric binary, based upon proper motion data collected during the Hipparcos mission. The visible component shows the spectrum of an evolved K-type giant or bright giant star with a stellar classification of K0 II-III. The measured angular diameter, after correction for limb darkening, is . At an estimated distance of this star, this yields a physical size of about 14 times the radius of the Sun.

The star is drifting further from the Earth with a heliocentric radial velocity of +15.2 km/s. It is located near the ecliptic and thus is subject to lunar occultations. This is an aging giant/bright giant star with a stellar classification of G8II-III, and is most likely (97% chance) on the horizontal branch. It is around 350 million years old with 3.3 times the mass of the Sun.

Iota Cancri is a wide double star. The primary is a yellow-hued G-type bright giant star of magnitude 4.0, located 330 ± 20 light-years from Earth. It spent much of its stellar life as a B-type main sequence star before expanding and cooling to its current state as it spent its core hydrogen. The secondary is a white main sequence star of spectral type A3V and magnitude 6.57.

It is moving closer to the Earth with a heliocentric radial velocity of −8.2 km/s. This is a bright giant with a stellar classification of F5 II. Gray et al. (2001) classify it as F5 Ib–II metal-weak, with the metallic lines matching a class of F0 whereas hydrogen lines match an F5. It is around 62 million years old with a projected rotational velocity of 46.

Components of the γ Andromedae system (not to scale) γ1 Andromedae (A component) is a bright giant star with a spectral classification of K3IIb. It has an apparent visual magnitude of approximately 2.26. γ2 Andromedae (BC component), with an overall apparent visual magnitude of 4.84, is 9.6 arcseconds away from γ1 Andromedae at a position angle of 63 degrees. γ1 and γ2 have an orbital period of approximately 5,000 years.

Hercules has no first or second magnitude stars. However, it does have several stars above magnitude 4. Alpha Herculis, traditionally called Rasalgethi, is a triple star system, partly resolvable in small amateur telescopes, 359 light-years from Earth. Its common name means "the kneeler's head". The primary is an irregular variable star; it is a bright giant with a minimum magnitude of 4 and a maximum magnitude of 3.

It is moving closer to the Earth with a heliocentric radial velocity of −23 km/s. Houk (1978) assigned the spectral classification of this star as F1III, which suggests it is an F-type (yellow- white) star that has evolved away from the main sequence and expanded into a giant. However, Gray et al. (2001) found a class of F0 Ib-II, matching a supergiant/bright giant star.

The less massive companion orbits every 3.6 years and is apparently a B9.5 main sequence star, but the dynamics of the system suggest that it may actually be a pair of stars is a close orbit. The Cepheid primary pulsates regularly with a period of 6.79671 days. It is a yellow-white supergiant or bright giant that is 5.6 times as massive as the Sun and 2,500 times as luminous.

It is drifting further away with a radial velocity of +13.3 km/s. This object is an aging bright giant star with a stellar classification of G6IIb With the supply of hydrogen at its core exhausted, it has expanded to 12 times the radius of the Sun. The star is radiating 89 times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 5,197 K.

HR 6902 (also designated V2291 Oph) is a binary system located 790 light years away from the Sun in the Ophiuchus constellation. The system includes an orange bright giant star and a B-type main sequence star, forming an eclipsing binary of Zeta Aurigae type. The system is also surrounded by a warm circumstellar envelope and the spectra show silicon and carbon absorption up to a distance of 3.3 giant radii.

The spectrum of Xi2 Sagittarii yields a mixed stellar classification of G8/K0 II/III, showing traits of a G- or K-type giant or bright giant star. It has an estimated 3.36 times the mass of the Sun and about 14 times the Sun's radius. At an age of around 380 million years, it is radiating 676 times the Sun's luminosity from its photosphere at an effective temperature of 4,541 K.

This is a single- lined spectroscopic binary system with an orbital period of 28.7 years and an eccentricity of 0.65. The primary member, designated component A, is an orange-hued (K–type) bright giant with a stellar classification of K1II. The star is around 50 million years old with 7 times the mass of the Sun. Having exhausted the supply of hydrogen at its core, it has expanded to roughly 56 times the Sun's radius.

63 Cygni is a single star in the northern constellation of Cygnus, located around 1,030 light years away from Sun. It is visible to the naked eye as an orange-hued star with an apparent visual magnitude of 4.56. 63 Cyg is moving closer to the Earth with a heliocentric radial velocity of −26 km/s. This is an evolved star showing a stellar spectrum with mixed traits between a bright giant and supergiant.

19 Aurigae is a single star located approximately 3,600 light years away from the Sun in the northern constellation Auriga. It is visible to the naked eye as a faint, white-hued star with an apparent visual magnitude of 5.05. The star is moving closer to the Earth with a heliocentric radial velocity of 4.3 km/s. This is an evolved A-type bright giant star with a stellar classification of A5 II+.

This is a double star and possible binary system. The primary component has a stellar classification of G2 Ib/II, which places it on the borderline between the bright giant and lower luminosity supergiant stars. It has passed the first dredge-up and may be undergoind Cepheid-like pulsations. With more than four times the mass of the Sun, this is an evolved star that has reached its current stage after only 135 million years.

Houk and Swift (1999) have it classed as a G8II bright giant. This is a red clump giant, which indicates it is on the horizontal branch and is generating energy through helium fusion at its core. It has a high lithium abundance and displays a far infrared emission excess. The star is an estimated 510 million years old with 2.72 times the mass of the Sun and has expanded to 15 times the Sun's radius.

This is an aging bright giant/supergiant star with a stellar classification of K2 Ib-II. It is a suspected variable star of unknown type, with a brightness that has been measured ranging from 4.83 down to 4.87. HD 115211 is an estimated 40 million years old with 7.1 times the mass of the Sun. With the supply of hydrogen exhausted at its core, it has expanded to 123 times the Sun's radius.

This is an evolved K-type star with a stellar classification of K0 II-III, displaying a luminosity class with mixed traits of a bright giant (II) and a giant star (III). With the supply of hydrogen at its core exhausted, the star has expanded to 16.8 times the radius of the Sun. It is radiating 152 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,942 K.

HD 77912 has a peculiar velocity of , which may mark it as a runaway star. The stellar classification of HD 77912 is , indicating it is a bright giant with a mild overabundance of Barium. It has 4.6 times the mass of the Sun and has expanded to 33 times the Sun's radius. The star is radiating 1,168 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,899 K.

Tau4 Serpentis, Latinized from τ4 Serpentis, is a M-type bright giant star in the constellation of Serpens, approximately 520 light-years from the Earth. It is classified as a semiregular late-type variable star, and its magnitude varies between +5.89 and +7.07 with a period of approximately 100 days. τ4 is unique among the stars with the Bayer designation τ Serpentis as being the only one with no HR catalog number.

HD 157819 is the Henry Draper Catalogue designation for a star in the southern constellation of Ara. It is faintly visible to the naked eye at an apparent visual magnitude of 5.94 and is approximately distant from the Earth. The spectrum of this star fits a stellar classification of G8 II-III, indicating it is a G-type star that is somewhere between the giant and bright giant stages of its evolution.

When luminosity classes were added to the MK spectral classification scheme, Canopus was assigned class Iab indicating an intermediate luminosity supergiant. This was based on the relative strengths of certain spectral lines understood to be sensitive to the luminosity of a star. In the Bright Star Catalogue 5th edition it is given the spectral class F0II, the luminosity class indicating a bright giant. Balmer line profiles and oxygen line strengths indicate the size and luminosity of Canopus.

Based upon parallax measurements, the star is located approximately 830 light years away from the Sun. It is moving closer to the Earth with a heliocentric radial velocity of −16 km/s. This is an aging bright giant star with a stellar classification of K2.5IIb, having exhausted the supply of hydrogen at its core and expanded to 100 times the radius of the Sun. It is 64 million years old with 6.2 times the Sun's mass.

Epsilon Leonis has a stellar classification of G1 II, with the luminosity class of II indicating that, at an age of , it has evolved into a bright giant. It is much larger and brighter than the Sun with a luminosity 288 times and a radius 21 times solar. Consequently, its absolute magnitude is actually –1.49, making it one of the more luminous stars in the constellation, significantly more than Regulus. Its apparent brightness, though, is only 2.98.

This object has a stellar classification of G4 Ib-II, matching a G-type star with a luminosity class part way between a bright giant and a supergiant star. It is just 90 million years old with around five times the mass of the Sun. The star has expanded to 48 times the Sun's radius and is radiating 1,087 times as much luminosity as the Sun from its enlarged photosphere at an effective temperature of 4,804 K.

The system is moving closer to the Earth with a heliocentric radial velocity of –23 km/s. The primary component of this system is a magnitude 5.31 K-type giant star or bright giant with a stellar classification of K1. The star is radiating 155 times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 4,660 K. Orbiting at an angular separation of 3.25 arcseconds is a magnitude 8.76 companion star.

It is moving closer to the Earth with a heliocentric radial velocity of –5 km/s. The stellar classification of this star is B8 II-III, with the luminosity class of II-III suggesting that the spectrum displays elements of both a giant star and a bright giant. It is a chemically peculiar star of the Mercury-Manganese type (CP3). This is a probable Alpha2 Canum Venaticorum variable that ranges in visual magnitude from 5.06 down to 5.16.

This is a single-lined spectroscopic binary star system with an orbital period of 207.357 days and an eccentricity of 0.55. The primary component has the spectrum of an evolved F-type giant/bright giant hybrid with a stellar classification of F7 II/III. It is around 46 million years old with 6.9 times the mass of the Sun. The star is radiating 3,919 times the Sun's luminosity from its photosphere at an effective temperature of 6,495 K.

The star has a peculiar velocity of relative to its neighbors, and may be a runaway star. This object is a bright giant star with a stellar classification of K2-IIb. It is a suspected variable star of unknown type with a brightness that has been measured varying from 4.73 down to 4.78. The star is about 61 million years old with 6.4 times the mass of the Sun and is spinning with a projected rotational velocity of 3.5.

Delta Sagittae (Delta Sge, δ Sagittae, δ Sge) is a binary star in the constellation of Sagitta, with an apparent magnitude of +3.68. The primary component is a red M-type bright giant, and the secondary is a B-type main- sequence star. It is approximately 430 light years from Earth, based on its Gaia Data Release 2 parallax. Delta Sagittae is a spectroscopic binary with a composite spectrum, meaning that light from both stars can be detected.

There has been some uncertainty as to the classification of this stage. Houk (1979) lists a stellar class of B8 Ib/II for HD 161840, which corresponds to a B-type bright giant/lesser supergiant mix. Multiple studies still use an older classification of B8 V, suggesting instead this is a B-type main-sequence star. Garrison and Gray (1994) assigned it a class of B8 III-IV, which would put it on the subgiant/giant star track.

The binary nature of this system was first detected as an ultraviolet excess in 1996. No radial velocity variation has been detected so it must be a wide system with an orbital period of up to 21 years. The estimated semimajor axis of their orbit is . The pair were not resolved using the Hubble Space Telescope WFPC2 instrument. The primary is an evolved bright giant star with a yellow-white hue and a stellar classification of F8II.

Beta Indi, Latinized from β Indi, is the second brightest star in the southern constellation of Indus. It is visible to the naked eye as a faint, orange-hued point of light with an apparent visual magnitude of 3.67. The star is located approximately 600 light years from the Sun, based on parallax, but is drifting closer with a radial velocity of −5 km/s. The stellar classification of this star is K1II, matching an evolved bright giant.

It is an orange- hued star of spectral type K3Ib-IIa that has been classified as a supergiant or bright giant, that is around 650 light-years from Earth. It is around 8.21 times as massive and 5,636 times as luminous as the Sun. At apparent magnitude 2.85, this difference in brightness between the two is undetectable by the unaided eye. Close to Beta Arae is Gamma Arae, a blue-hued supergiant of spectral type B1Ib.

Consequently, the Chinese name for ι Ceti itself is (, .) 香港太空館 - 研究資源 - 亮星中英對照表 , Hong Kong Space Museum. Accessed on line November 23, 2010. This is an MK-standard star with a stellar classification of K1.5 III, indicating that it is an evolved K-type giant star. However, Houk and Swift (1999) list a classification of K1 II, which would indicate this is a bright giant.

The brighter of the two, component Aa, is a blue-white B-type bright giant or main sequence star with an apparent magnitude of +5.08. It is around 43 million years old with six times the mass of the Sun. The star is radiating 238 times the Sun's luminosity from its photosphere at an effective temperature of 9,623 K. The third member, component B, is an eighth magnitude star at an angular separation of from the primary.

Based upon parallax measurements, Beta Pegasi is located about from the Sun. It is unusual among bright stars in having a relatively cool surface temperature compared to stars like the Sun. This star has a stellar classification of M2.3 II–III, which indicates the spectrum has characteristics partway between a bright giant and a giant star. It has expanded until it is some 95 times as large, and has a total luminosity of 1,500 times that of the Sun.

HD 112028 is an evolved star in the northern constellation of Camelopardalis. It has spectral peculiarities that have been interpreted as a shell, and also relatively weak magnesium and silicon lines. Its spectral class has been variously assigned between B9 and A2, and its luminosity class between a subgiant and bright giant. At an angular separation of 21.47″ is the slightly fainter spectroscopic binary HD 112014, consisting of a pair of A-type main sequence stars.

This relies on distance and luminosity estimates lower than most observations. The star would be an unusually large and bright giant star for the given mass, possibly as the result of very high mass loss. To match the observed eclipse and orbital data, the secondary is a fairly normal B main sequence star of about embedded in a thick disc seen nearly edge on. The orbit itself is now fairly well determined, inclined at over 87 degrees to Earth.

Xi Telescopii, Latinized from ξ Telescopii, is a solitary star in the southern constellation of Telescopium. It is visible to the naked eye, with an apparent visual magnitude of +4.95. Based upon an annual parallax shift of 3.02 mas as measured from Earth, it is located approximately 1,100 light years from the Sun. This is an evolved star with a stellar classification of K5 III or M1 IIab, indicating it is a giant or bright giant star.

Alpha Trianguli Australis is a bright giant star with an apparent magnitude of +1.91. Based upon parallax measurements, this star is located roughly distant from the Earth. The estimated age of the star is 48 million years old; sufficiently old for a massive star to evolve away from the main sequence and expand into a giant. It has a mass roughly seven times the mass of the Sun, but is emitting about 5,500 times the Sun's luminosity.

BE Camelopardalis is a solitary variable star in the northern circumpolar constellation of Camelopardalis. It is visible to the naked eye as a faint, red-hued point of light with an apparent visual magnitude that fluctuates around 4.39. The star is located roughly 800 light years away from the Sun based on stellar parallax. This object is an M-type bright giant with a stellar classification of M2 II, and is currently on the asymptotic giant branch.

Delta Volantis (δ Vol, δ Volantis) is a solitary star in the southern constellation Volans. It has an apparent visual magnitude of +3.97, which is bright enough to be seen with the naked eye. Based upon parallax measurements, is approximately 740 light years from the Sun. This is an F-type bright giant star with a stellar classification of F6 II. It has an estimated radius 24 times that of the Sun, and shines with more than a thousand times the Sun's luminosity.

It has an absolute magnitude of −1.45. This is an aging bright giant with a stellar classification of K0.5IIbCN1, where the suffix notation indicates an anomalous overabundance of cyanogen in the spectrum. It is a mild barium star, which may indicate it is on the asymptotic giant branch stage of its evolution. The star has expanded to 41 times the radius of the Sun and is radiating 677 times the Sun's luminosity from its swollen photosphere at an effective temperature of 4,584 K.

Its colour is obvious when seen through binoculars. It is a multiple system, consisting of the spectroscopic binary Gamma A and three optical companions, Gamma B, magnitude 13; Gamma C, magnitude 12; and Gamma D, magnitude 10. The two components of Gamma A orbit each other every 389.2 days, with an eccentric orbit that takes their separation between 2.3 and 1.4 astronomical units (AU). Epsilon Canis Minoris is a yellow bright giant of spectral class G6.5IIb of magnitude of 4.99.

Its spectral type is K0II, and it is of apparent magnitude 4.11. Since its formation, it has evolved from a B-type star to a K-type star. Its luminosity class places it as a bright giant; its luminosity is 730 times that of the Sun, designating it one of the highest-luminosity K0-type stars visible to the naked eye. 100 million years old, it has a radius of 43 solar radii () and a mass of between 4.5 and 5 solar masses ().

This is a bright giant star with a stellar classification of K2.5 II. It is a slow irregular variable of type LC with a frequency of 0.16585 cycles per day. In the R (red) band, the magnitude of the star ranges from 3.43 down to 3.81. The measured angular diameter of this star, after correction for limb darkening, is . At the estimated distance of GZ Vel, this yields a physical size of about 140 times the radius of the Sun.

The system is moving further from the Earth with a heliocentric radial velocity of +1.1 km/s. The magnitude 5.88 primary, component A, is itself a binary star with a separation of – and an orbital period of around . The brighter member of this duo is a G-type bright giant with a stellar classification of G4 II and 2.6 times the mass of the Sun. Its companion is an early A-type star with double the mass of the Sun.

The stellar classification of this star is B5 II/III, which matches the spectrum of a giant/bright giant although stellar models suggest it may still be on the main sequence. It has over four times the mass of the Sun and is 291 million years old. The star has a high rate of spin, showing a projected rotational velocity of 116 km/s. It is radiating around 489 times the luminosity of the Sun from its photosphere at an effective temperature of .

It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 4.244. This object is located 280 light years away and is moving further from the Earth with a heliocentric radial velocity of +8 km/s. It is a candidate member of the Hyades Supercluster. This is an aging K-type star with a stellar classification of K2 II-III, showing a luminosity class with blended traits of a giant and a bright giant.

This is an aging K-type giant/bright giant with a stellar classification of K2II/III. With the supply of hydrogen at its core exhausted, the star expanded and cooled. It now has 30 times the radius of the Sun and is radiating 287 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,322 K. The star was first designated Lambda Chamaeleontis by French astronomer Lacaille, in his Coelum Australe Stelliferum. He listed it close to Pi Chamaeleontis in both brightness and location.

The two stars are close enough that periodic Doppler shifts in their spectra can be made out. In this case, light from both stars can be detected (and they overlap in the spectrum), so it is a double-lined system. The primary star, designated HD 25555, is a K-type bright giant, and the secondary star, designated HD 25556, is a B-type main-sequence star. However, the spectrum has also been interpreted as a G-type star and an A-type main- sequence star.

South of Delta is Gamma Lyrae, a blue giant and the second-brightest star in the constellation. Around 190 parsecs distant, it has been referred to as a "superficially normal" star. The final star forming the lyre's figure is Beta Lyrae, also a binary composed of a blue bright giant and an early B-type star. In this case, the stars are so close together that the larger giant is overflowing its Roche lobe and transferring material to the secondary, forming a semidetached system.

RR Lyrae itself varies between magnitudes 7 and 8 while exhibiting the Blazhko effect. The easternmost star designated by Flamsteed, 19 Lyrae, is also a small-amplitude variable, an Alpha2 Canum Venaticorum variable with a period of just over one day. Another evolved star is the naked-eye variable XY Lyrae, a red bright giant just north of Vega that varies between 6th and 7th magnitudes over a period of 120 days. Also just visible to the naked eye is the peculiar classical Cepheid V473 Lyrae.

It is drifting further away with a radial velocity of +19 km/s. This evolved object has received stellar classifications of A7Ia and A6II, indicating that it is a massive supergiant or bright giant star. It has 7.8 times the mass of the Sun and is around 40 million years old. The star has expanded to nearly 34 times the girth of the Sun and is radiating around 4,140 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 7,977 K.

The star has an absolute magnitude of −3.77, and is drifting further away with a radial velocity of +9.9 km/s. This object is a massive, aging bright giant with a stellar classification of K3II-IIb. It is a suspected variable star that fluctuates in magnitude by an amplitude of 0.05 in the B-band of the UBV photometric system. With the supply of hydrogen exhausted at its core, it has evolved of the main sequence and cooled and expanded to 156 times the Sun's radius.

O. J. Eggen identified it as a member of the Pleiades group of co-moving stars. This object is a massive bright giant star with a stellar classification of B5 II. It is 25 million years old and is spinning with a projected rotational velocity of 19 km/s. The star has 9 times the mass of the Sun and about 18 times the Sun's radius. It is radiating 11,634 times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 14,300 K.

The light curve of this magnitude change follows a regular saw-tooth pattern. During each radial pulsation cycle, the radius of the star varies by ±3.9 times the Sun's radius around a mean of 67.8. Its spectral type and luminosity class are likewise variable, from F-type to G-type and from a supergiant to a bright giant. Far ultraviolet emissions have been detected from this star with the Far Ultraviolet Spectroscopic Explorer, while X-ray emissions were detected with the XMM-Newton space telescope.

Zeta Aurigae is an eclipsing binary with the orbital plane being oriented close to the line of sight from the Earth; the inclination of this system is estimated as 87.0°. As a result, an eclipse of one star by the other occurs during each orbit, causing the magnitude to decrease to +3.99. The pair have an orbital period of 972 days (2.66 years) and an eccentricity of 0.4. The primary component, Zeta Aurigae A, has been categorized as a K-type bright giant or supergiant star.

CG Andromedae is also a chemically peculiar star with a strong magnetic field, or Ap star, with a spectral type A0IIspSiSrHg. This means that it's a bright giant star that shows narrow absorption lines and unusual strong lines of silicium, strontium and mercury. Calcium and manganese lines are weaker than expected instead. Other sources report that the stronger lines are of silicium and europium, thus giving a spectral classification B9pSiEu, which has just a slightly different temperature for the blackbody emission in addition to the different lines.

It forms a suspected ellipsoidal variable with a period of 80 days and an amplitude variation of 0.08 in magnitude. The primary component is an aging red giant/bright giant with a stellar classification of M1/M2II/III, currently on the asymptotic giant branch. With the supply of hydrigen at its core exhausted, it has expanded to 160 times the girth of the Sun. It is radiating 3,562 times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 3,562 K.

Canopus , also designated α Carinae, Latinised to Alpha Carinae, is the brightest star in the southern constellation of Carina and the second- brightest star in the night sky. With a visual apparent magnitude of −0.74, it is outshone only by Sirius. Located around from the Sun, Canopus is a bright giant of spectral type A9, so it is essentially white when seen with the naked eye. It has a luminosity over 10,000 times the luminosity of the Sun, is eight times as massive, and has expanded to 71 times the Sun's radius.

Gray and Garrison (1989) listed a stellar classification of F2 II/III for this star, suggesting it is a K-type star with a spectrum showing mixed traits of a giant/bright giant. Houk and Smith-Moore (1978) had a similar classification of F2/3 II/III. This may indicate it is not a member of NGC 6530, since it shouldn't have evolved to this class from the O-type stars that still populate this cluster, and hasn't had time to evolve from a less massive cluster star.

The spectrum of the primary component displays a stellar classification of K1 Ib–II, indicating this is a K-type star with a mixed luminosity class of an evolved bright giant/supergiant star. It is a mild barium star, showing an enhanced abundance of s-process elements in its outer atmosphere. This material was most likely acquired during a previous mass transfer from its now white dwarf companion. The primary has an estimated 1.4 times the mass of the Sun and has expanded to 85 times the Sun's radius.

Eta Columbae is a solitary star near the southern boundary of the constellation Columba. It is visible to the naked eye, having an apparent visual magnitude of 3.96. Based upon an annual parallax shift of 6.91 mas, it lies at a distance of roughly 472 light years from the Sun. This is an orange- hued K-type giant star with a stellar classification of K0 III, or possibly a bright giant with a crossover class of G8/K1 II. The measured angular diameter of this star, after correction for limb darkening, is .

Theta Herculis is a single, variable star in the northern constellation of Hercules. This object is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 3.851. Based upon parallax measurements, it is located around 750 light years away from the Sun. The star is advancing toward the Earth with a heliocentric radial velocity of –28 km/s. This is an aging K-type bright giant with a stellar classification of K1IIaCN2, where the suffix notation indicates a strong overabundance of CN in the spectrum.

This is an evolved bright giant star with a stellar classification of F7/8 II. The spectrum displays a deficit of carbon, an excesses of nitrogen, and a high abundance of lithium. The first two anomalies suggest the giant has passed through a deep convection stage that would have also exhausted the lithium supply, indicating the current lithium abundance is of recent production. The star has 2.7 times the mass of the Sun and is radiating 515 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 5,868 K.

Theta Lyrae (θ Lyr) is a star in a trinary star system, in the constellation Lyra, approximately 770 light years away from Earth. Theta Lyrae is an orange bright giant star of the spectral type K0II, which means that it possesses a surface temperature of about 5,000 kelvins, and is many times bigger and brighter, yet cooler, than the Sun. It is orbited by a subsystem composed of BD+37° 3399 and BD+37° 3399B. 10th magnitude BD+37° 3399 is a giant star with a spectral type of K2III.

This star has received a stellar classification of G8Iab, which suggests it is a G-type supergiant star, as well as G7.5II-IIICN0.5, which instead indicates a luminosity class between a giant and a bright giant. Abundance analysis suggests the star has not yet passed the first dredge-up. It has 4.6 times the mass of the Sun and has expanded to 33 times the Sun's radius. The star is radiating 627 times the luminosity of the Sun from its photosphere at an effective temperature of 4,837 K.

It has 12 times the mass of the Sun and has expanded to 202 times the Sun's radius. The star is radiating 8,478 times the luminosity of the Sun from its bloated photosphere at an effective temperature of 3,900 K. The magnitude 7.48 companion star, component B, was discovered by J. Dunlop in 1829. As of 2015, it was located at an angular separation of along a position angle of 21°, relative to the primary. It is a B-type giant/bright giant star with a class of B9II/III.

This object has a stellar classification of K0.5IIb, which indicates it is an evolved bright giant. With the supply of hydrogen at its core exhausted, the star has expanded to 51 times the Sun's radius. It is radiating around 919 times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 4,471 K. It is generally deficient in metal elements, but appears weakly enhanced in barium and other heavier elements. This is a suspected barium star and hence may have a white dwarf companion in orbit.

Its light is dimmed by 30% due to interstellar dust, so would have a brighter magnitude of 3.31 if not for this. The second brightest star at magnitude 3.97 is Beta Pyxidis, a yellow bright giant or supergiant of spectral type G7Ib-II that is around 435 times as luminous as the Sun, lying 420 ± 10 light-years distant away from Earth. It has a companion star of magnitude 12.5 separated by 9 arcseconds. Gamma Pyxidis is a star of magnitude 4.02 that lies 207 ± 2 light- years distant.

A view of Alpha Herculis in a small telescope. The components A and B are resolved with angular separation of 4.64 (in 2020). Alpha Herculis A and B are more than 500 AU apart, with an estimated orbital period of approximately 3600 years. A presents as a relatively massive red bright giant, but radial velocity measurements suggest a companion with a period of the order of a decade. B's two components are a primary yellow giant star and a secondary, yellow-white dwarf star in a 51.578 day orbit.

Beta Corvi has about 3.7 times the Sun's mass and is roughly 206 million years old, which is old enough for a star of this mass to consume the hydrogen at its core and evolve away from the main sequence. The stellar classification is G5 II, with the luminosity class of 'II' indicating this is a bright giant. The effective temperature of the star's outer envelope is about 5,100 K, which produces a yellow hue common to G-type stars. The measured angular diameter of this star is .

Barry (1970) assigned this star a stellar classification of F3 V, indicating an ordinary F-type main-sequence star. However, Houk and Swift (1999) classified it as A9 Ib/II, suggesting instead that this is an evolved F-type bright giant/supergiant. It is about one billion years old and is spinning with a projected rotational velocity of 77.7 km/s. The star has an estimated 1.58 times the mass of the Sun and is radiating 7.7 times the Sun's luminosity from its photosphere at an effective temperature of 6,952 K.

Gamma Canis Majoris is a blue- white B-type bright giant with a stellar classification of B8II and an apparent magnitude of +4.11. It is approximately 440 light years from Earth. It is a chemically peculiar Hg-Mg star displaying abnormal lines of mercury and magnesium. This star has 5.6 times the radius of the Sun and the outer atmosphere has an effective temperature of 13,596 K. This star is suspected of being a spectroscopic binary system, and there is a candidate companion at an angular separation of 0.332″ along a position angle of 114.8°.

The spectrum, mass, and luminosity is dominated by component Aa which is now considered to be an O9 bright giant. It is thought to have a mass around , a temperature of 32,000 K, and a luminosity of . The two eclipsing stars are almost identical class B main sequence stars with masses around . This star is sometimes known as the 'Mexican Jumping Star' by amateur astronomers, because it can appear to 'jump around' with respect to the other stars in the cluster because of its marked contrast in brightness.

This is the brightest star in the vicinity of the open cluster NGC 2287, although it is probably not a member based on its proper motion. This star has a stellar classification of B7 II/III, matching a B-type giant/bright giant hybrid. (Cidale et al. (2007) show a class of B5 V, which would indicate it is instead a B-type main-sequence star.) It is a magnetic Bp star of the helium–weak variety (CP4), with the spectrum displaying evidence for vertical stratification of helium in the atmosphere.

Epsilon Canis Minoris (ε Canis Minoris) is a suspected binary star system in the equatorial constellation of Canis Minor. It is a fifth magnitude star, which means it is bright enough to be faintly visible to the naked eye. Based upon an annual parallax shift of just 3.13 mas as seen from Earth, this star is located roughly 770 light years from the Sun, give or take a 40 light year margin of error. This is an evolved G-type bright giant star with a stellar classification of G6.5 IIb.

It is most likely (99% chance) on the horizontal branch, and is a barium star that shows an abnormal overabundance of barium in its spectrum. This s-process element may have been accreted from a now white dwarf companion during a previous stage of its evolution. The bright giant component has an estimated 4.63 times the mass of the Sun and has expanded to 45.5 times the Sun's radius. The star is radiating 1,087 times the Sun's luminosity from its enlarged photosphere at an effective temperature of about 4,916 K.

They share a common motion through space and thus appear to be physically associated, with a wide projected separation of or greater. If they are bound in an orbit, the estimated period is approximately 28,000 years. The brighter member of this system is an aging giant or bright giant star with a stellar classification of K0II-III. It has exhausted the supply of hydrogen at its core and expanded to 20 times the girth of the Sun. This is a suspected variable that has been recorded ranging in brightness from magnitude 4.98 down to 5.06.

Rho Persei is a semiregular variable star, whose apparent magnitude varies between 3.3 and 4.0 with periods of 50, 120 and 250 days. The star has reached the asymptotic giant branch of its evolution. It is a bright giant star with a stellar classification of M4 II. The outer envelope has an effective temperature of 4,111 K, giving it the red-orange hue of an M-type star. This star has a mass five times the mass of the Sun, while its radius has expanded to 150 times solar.

Low-amplitude radial velocity variations with a period of 613 days in the bright giant have suggested the possible presence of a substellar companion. If this is really due to a low-mass object, such a companion would be as small as 0.027 Solar masses (27 times the mass of Jupiter, probably a brown dwarf) and 3 astronomical units away from the bright primary. A substellar companion is only one of several hypotheses to explain the star's behaviour. Most likely the cause of the variation is weak pulsation of the star's atmosphere.

Beta Camelopardalis, Latinized from β Camelopardalis, is the brightest star in the northern constellation of Camelopardalis. It is bright enough to be faintly visible to the naked eye, having an apparent visual magnitude of 4.02. Based upon an annual parallax shift of 3.74 mas as seen from Earth, it is located roughly 870 light years from the Sun. It is moving closer with a radial velocity of −190 km/s and is most likely a single star. This is a yellow-hued G-type supergiant/bright giant with a stellar classification of G1 Ib–IIa.

Psi Ophiuchi, which is Latinized from ψ Ophiuchi, is a single star in the equatorial constellation of Ophiuchus, located next to the western constellation border with Scorpius. It has an orange hue and is visible to the naked eye as a faint point of light with an apparent visual magnitude of 4.50. The distance to this object is approximately 199 light years based on parallax. This is an aging giant or bright giant star with a stellar classification of K0- II-III, which indicates it has exhausted the supply of hydrogen at its core then cooled and expanded.

Between 240,000 and 270,000 times as luminous as the Sun, it is around 9,160 light-years distant from Earth.Table 4 in AO Cassiopeiae is a binary system composed of an O8 main sequence star and an O9.2 bright giant that respectively weigh anywhere between 20.30 and 57.75 times and 14.8 and 31.73 times the mass of the Sun. The two massive stars are so close to each other they distort each other into egg-shapes. Tycho Brahe's supernova was visible within Cassiopeia, and the star Tycho G is suspected of being the donor of the material that triggered that explosion.

This is an evolved bright giant star with a stellar classification of G5 II. It is positioned near the instability strip and in 1977 was listed as a candidate cepheid variable star with a luminosity amplitude of 0.086 and a period of 0.7282 days. The interferometer-measured angular diameter of this star is . At its estimated distance, this yields a physical size of about 72 times the radius of the Sun. It has 6.3 times the mass of the Sun and radiates 1,813 times the solar luminosity from its outer atmosphere at an effective temperature of 5,090 K.

It has the uncommon traditional name Ghusn al Zaitun, from the Arabic الغصن الزيتون al-ghuşn al- zaitūn "the olive branch" (carried by the dove of Noah's Ark). This is a single-lined spectroscopic binary system with an orbital period of 868.78 days and an eccentricity of 0.7. It has a peculiar velocity of , making it a candidate runaway star system. The primary component is a G-type bright giant star with a stellar classification of G7 II. It radiates around 149 time the solar luminosity from its outer atmosphere at an effective temperature of 5,136 K.

These stars mark the paws of the Lesser Dog's left hind leg, while magnitude 5.13 Zeta marks the right. A blue-white bright giant of spectral type B8II, Zeta lies around away from the Solar System. Lying 222 ± 7 light-years away with an apparent magnitude of 4.39, HD 66141 is 6.8 billion years old and has evolved into an orange giant of spectral type K2III with a diameter around 22 times that of the Sun, and weighing 1.1 solar masses. It is 174 times as luminous as the Sun, with an absolute magnitude of −0.15.

At Iota Aurigae's distance, extinction from interstellar dust is causing a magnitude reduction of about 0.6. Examination of the spectrum yields a stellar classification of K3 II, with the luminosity class of 'II' indicating this is a category of evolved star known as a bright giant. Since 1943, the spectrum of this star has served as one of the stable anchor points by which other stars are classified. The effective temperature of the outer envelope is 4,160 K, which is cooler than the Sun's effective temperature and gives Iota Aurigae the orange hue of a K-type star.

This is a Classical Cepheid variable with an apparent magnitude that ranges from 6.33 to 6.90 over 3.38926 days. It is a bright giant/supergiant with a nominal stellar classification of F7 Ib/II, but pulsates between spectral types F5Ib/II-G5. Depending on the method employed, the estimated mass is 5.42 or 5.66 times the mass of the Sun and it has 24.7 or 35.8 times the Sun's radius. R TrA has an infrared excess that is being emitted by circumstellar silicate dust heated to 150–200 K. It is losing mass at the rate of .

Its distance from Earth is roughly , based upon parallax measurements with an 11% margin of error. The primary component of this system has a magnitude of 5.27 and a stellar classification of G3 II, which suggests this is an evolved star in the bright giant stage. The companion is an A-type main sequence star with a stellar classification of A2 V. As of 2010, it is located at an angular separation of 0.1843 arcseconds along a position angle of 135.1°. They orbit each other with an estimated period of 201 years and a semimajor axis of 0.45 arcseconds.

Beta Arae (β Ara, β Arae), the brightest star in the constellation of Ara, is a very luminous, relatively young, giant star with an apparent visual magnitude of 2.8 (rounded). Parallax measurements place it at roughly from Earth. The spectrum of this star matches a stellar classification of K3 Ib- IIa, with the luminosity class notation 'Ib-IIa' indicating that the star lies part way between a higher luminosity bright giant (IIa) and a lower luminosity supergiant (Ib). This represents two of the evolutionary stages that a massive star passes through after it has exhausted the hydrogen at its core.

Lyra with the δ Lyrae pair and surrounding cluster stars left of centre Delta2 Lyrae (δ2 Lyr) is a 4th magnitude star in the constellation Lyra, approximately 900 light years away from Earth. It is one of the M4II spectral standard stars, meaning it is a bright giant star with a surface temperature around 3,600 kelvins. It puts out more energy than 10,000 suns, although more than 90% of it at longer than visual wavelengths. Direct angular measurements, combined with the Hipparcos parallax, give a radius of 1.1 \- 1.3 astronomical units, comparable to the size calculated from other observed data.

Phi Capricorni (φ Cap, φ Capricorni) is a solitary star in the southern constellation of Capricornus. It is visible to the naked eye with an apparent visual magnitude of +5.16. Based upon an annual parallax shift of 5.07 mas as seen from the Earth, the star is located about 640 light years from the Sun, give or take 30 light years. This is an evolved, orange-hued K-type giant/bright giant star with a stellar classification of K0 II-III It shows an infrared excess, which may be due to leftover material from a mass-loss event.

Beta Coronae Australis, Latinized from β Coronae Australis, is a single star in the southern constellation of Corona Australis. It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 4.10. The star is located around 470 light years distant from the Sun based on parallax, and is drifting further away with a radial velocity of +3 km/s. This is an aging K-type giant/bright giant star with a stellar classification of K0II/IIICNIb, where the suffix notation indicates an abundance anomaly of CN in the spectrum.

Omega Hydrae, Latinized from ω Hydrae, is a golden-hued star in the equatorial constellation of Hydra, located to the west-southwest of the brighter star Zeta Hydrae. Based upon an annual parallax shift of just 3.64 mas as seen from Earth, it is located roughly 900 light years from the Sun. It is faintly visible to the naked eye with an apparent visual magnitude of 5.00. This is an evolved K-type star with a stellar classification of K2 II-III, which indicates a spectrum showing traits intermediate between the giant and bright giant stages.

AO Cassiopeiae, also known as Pearce's Star, is a binary system composed of an O8 main sequence star and an O9.2 bright giant that respectively weigh anywhere between 20.30 and 57.75 times and 14.8 and 31.73 times the mass of the Sun. The AO Cas system is an eclipsing binary with a period of roughly 3.5 days, with the apparent magnitude ranging between 6.07 and 6.24. Stars of this brightness are generally just visible to the unaided eye in dark skies in semirural locations. The component stars are so close to each other they are ellipsoidal (egg-shaped).

Based upon parallax measurements, Alpha Sagittae is approximately 382 light-years from the Sun. It is moving further away from the Earth with a heliocentric radial velocity of 1.7 km/s. This is an evolved bright giant with a stellar classification of G1 II. It is 151 million years old with 4 times the mass of the Sun and has expanded to around 21 times the Sun's radius. It is radiating 340 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 5,333 K. There is an X-ray source within of these coordinates.

Of apparent magnitude 5.11, the yellow bright giant Kappa Trianguli Australis of spectral type G5IIa lies around distant from the Solar System. Eta Trianguli Australis (or Eta1 Trianguli Australis) is a Be star of spectral type B7IVe which is from Earth, with an apparent magnitude of 5.89. Lacaille named a close-by star as Eta as well, which was inconsistently followed by Francis Baily, who used the name for the brighter or both stars in two different publications. Despite their faintness, Benjamin Gould upheld their Bayer designation as they were closer than 25 degrees to the south celestial pole.

Traditionally known as Pherkad, Gamma Ursae Minoris has an apparent magnitude that varies between 3.04 and 3.09 roughly every 3.4 hours. It and Kochab have been termed the "guardians of the pole star". A white bright giant of spectral type A3II- III, with around 4.8 times the Sun's mass, 1,050 times its luminosity and 15 times its radius, it is 487±8 light-years distant from Earth. Pherkad belongs to a class of stars known as Delta Scuti variables—short period (six hours at most) pulsating stars that have been used as standard candles and as subjects to study asteroseismology.

The star system, appearing as one star, is deemed visible to the naked eye with its combined apparent visual magnitude of 4.41. Based upon an annual parallax shift of 7.74 mas as seen from Earth, this system is about 420 light years from the Sun, much further than Nu1 and Nu2 which appear nearby when seen from one point in our solar system. The primary member, component A, is an evolved, orange-hued giant/bright giant hybrid with an apparent magnitude of +4.63 and a stellar classification of K0 II-III. It is most likely (96% chance) on the horizontal branch.

The spectrum of the system's primary, Pi Sagitarii A, matches a stellar classification of F2 II. The 'II' luminosity class is for a bright giant star that has exhausted the hydrogen at its core and has followed an evolutionary track away from the main sequence of stars like the Sun. Because it has nearly six times the mass of the Sun, it reached this stage in a mere 67 million years. The outer envelope is radiating energy at an effective temperature of about 6,590 K, giving it the yellow-white hue of an F-type star. Pi Sagittarii A has two nearby companions.

Beta¹ Capricorni is the more complex of the pair and has a spectrum that is difficult to interpret. Its dominant pair of stars are the orange K-type bright giant Beta Capricorni Aa, with an apparent magnitude of +3.08, and the blue-white B-Type main sequence dwarf Beta Capricorni Ab1 with an apparent magnitude of +7.20. They are separated by 0.05 arcseconds (5 AU) and have an orbital period of 3.77 years. The Aa component has a surface temperature of 4900 kelvins, a radius 35 times that of the Sun, and a luminosity 600 times that of the Sun.

This is a white A-type bright giant with a stellar classification of A4II/III. It is one of the brighter members of this rare class of stars, making it of interest for study. Omicron Scorpii has about eight times the mass of the Sun, fifteen times the radius, and is roughly 40 million years old. The star is radiating around 3,200 times the luminosity of the Sun from its outer atmosphere at an effective temperature of about 8,128 K. It does not display an infrared excess due to circumstellar dust or a possible infrared-bright companion, but the light from this star is subject to extinction from interstellar dust.

The primary component is a peculiar bright giant with a stellar classification of . This notation indicates it is a K-type giant with some uncertainty about the classification, along with an overabundance of barium and underabundances of the CN and CH radicals. It is an active star, roughly 100 million years old, with 5.4 times the Sun's mass. The star has expanded to 40 times the radius of the Sun and is radiating 680 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,416 K. The system displays an excess of ultraviolet radiation that must be coming from the secondary companion.

This is a single-lined spectroscopic binary star system with an orbital period of 2.9 years and an eccentricity of 0.48. The primary member, component A, is an evolved bright giant with a stellar classification of kA5hF0mF5 II. This notation indicates the star's spectrum shows the calcium K lines of an A5 star, the hydrogen lines of an F0 star, and the metallic lines of an F5 star. It is an evolved Am star of the ρ Puppis type, a class of evolved stars showing the Am chemical peculiarities. It is located in the instability strip of the Hertzsprung–Russell diagram but is not thought to be variable.

The system is moving further from the Earth with a heliocentric radial velocity of +20 km/s. The primary component of this system, HD 92449, is a bright giant with a stellar classification of G5 IIa. The star radiates 1,370 times the Sun's luminosity from its photosphere at an effective temperature of 5,100 K. It shares a common proper motion with the magnitude 6.06 star HD 92463, and the pair likely form a binary system. This secondary component is a B-type main-sequence star with a class of B8 V. As of 2000, it had an angular separation of along a position angle of 105° from the primary.

Pi Aurigae, Latinized from π Aurigae, is the Bayer designation for a single, red-hued star in the northern constellation of Auriga. Located about one degree north of the 2nd magnitude star Beta Aurigae, Pi Aurigae is visible to the naked eye with an apparent visual magnitude of 4.25 Based upon parallax measurements, it is approximately away from Earth. At that distance, the brightness of the star is diminished by 0.54 in magnitude from extinction caused by interstellar gas and dust. Pi Aurigae is an evolved bright giant star with a stellar classification of M3 II. The measured angular diameter of this star, after correction for limb darkening, is .

Stars that would be brighter than this shed their outer layers so rapidly that they remain hot supergiants after they leave the main sequence. The majority of red supergiants were main sequence stars and now have luminosities below , and there are very few bright supergiant (Ia) M class stars. The least luminous stars classified as red supergiants are some of the brightest AGB and post-AGB stars, highly expanded and unstable low mass stars such as the RV Tauri variables. The majority of AGB stars are given giant or bright giant luminosity classes, but particularly unstable stars such as W Virginis variables may be given a supergiant classification (e.g.

In defining the constellation, Lacaille gave twelve stars Bayer designations of Alpha through to Lambda, with two close stars called Eta (one now known by its Henry Draper catalogue number), while Lambda was later dropped due to its dimness. The three brightest stars, Alpha, Beta and Gamma, make up the triangle. Readily identified by its orange hue, Alpha Trianguli Australis is a bright giant star of spectral type K2 IIb-IIIa with an apparent magnitude of +1.91 that is the 42nd-brightest star in the night sky. It lies away and has an absolute magnitude of −3.68 and is 5,500 times more luminous than our Sun.

The primary (θ Scorpii A) is an evolved bright giant star with a stellar classification of F0 II. With a mass 5.7 times that of the Sun, it has expanded to about 26 times the Sun's radius. It is radiating 1,834 times as much luminosity as the Sun from its outer envelope at an effective temperature of 7,268 K, giving it the yellow-white hued glow of an F-type star. This star is rotating rapidly, giving it an oblate shape with an equatorial radius 19% larger than the polar radius. Artistic impression The magnitude 5.36 companion (θ Scorpii B) is at an angular separation of 6.470 arcseconds.

Keenan and McNeil (1989) listed a stellar classification of G7 II-III for 24 Cep, matching the spectrum of an evolved G-type star with blended features of a bright giant and a giant star. Older sources list a class of G8 III, which would suggest an ordinary giant star. At the age of 234 million years, it has an estimated 3.5 times the mass of the Sun and has expanded to about 13 times the Sun's radius. The star is radiating 199 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 5,023 K. These coordinates are a source of X-ray emission.

Beta Scuti, Latinized from β Scuti, is a binary star system in the southern constellation Scutum. Based upon an annual parallax shift of 3.56 mas as seen from Earth, it is located approximately 920 light years from the Sun. The primary component has an apparent visual magnitude of +4.22 and is radiating about 1,270 times the luminosity of the Sun from its outer atmosphere at an effective temperature of 4,622 K. This yellow-hued star is a G-type bright giant with a stellar classification of G4 IIa. This is a spectroscopic binary with an orbital period of 2.3 years and eccentricity around 0.35.

The star Pi Herculis, rendered with Celestia software, as it might appear from 3 Astronomical Units away. Pi Herculis is a bright giant star with a stellar classification of K3 II. P.C. Keenan and R. E. Pitts (1980) graded it as a spectral type K3 IIab and it is sometimes listed with this alternate classification. The star is enormous compared to the Sun, having a mass that is 4.5 times solar and a radius approximately 60 times depending on which wavelength the star's angular diameter is measured at. Due to limb darkening, all giant and supergiant stars present unique challenges when measuring their photosphere.

Position of γ Aquilae relative to upright Gamma Aquilae is a relatively young star with an age of about 100 million years. Nevertheless, it has reached a stage of its evolution where it has consumed the hydrogen at its core and expanded into what is termed a bright giant star, with a stellar classification of K3 II. The star is now burning helium into carbon in its core. After it has finished generating energy through nuclear fusion, Gamma Aquilae will become a white dwarf. The interferometry-measured angular diameter of Gamma Aquilae is mas, which, at its estimated distance, equates to a physical radius of about 95 times the radius of the Sun.

This is an aging bright giant star with a stellar classification of G0II. It is a candidate Cepheid variable, but Hipparcos photometry found its brightness to be constant. The star has expanded to 22 times the radius of the Sun and is radiating 283 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 5,051 K. It has a magnitude 13.0 visual companion at an angular separation of along a position angle of 313° relative to the brighter component, as of 2000. HD 102350 is listed in the Washington Double Star Catalog as having a 13th magnitude companion about away, but it is a distant background object unrelated to HD 102350.

The stellar classification of this star, G4 II–III, places it midway between the giant and bright giant stages of its evolution. The interferometry-measured angular diameter of this star is about 2.42 mas, which, at its estimated distance, equates to a physical radius of about 14 times the radius of the Sun. It has about three times the mass of the Sun and radiates 138 times the Sun's luminosity from its outer atmosphere at an effective temperature of 5,282 K, giving it the yellowish hue of a G-type star. In 1963, East German astronomer Gerhard Jakisch reported this star as a variable with a period of 358 days and an amplitude of 0.08 magnitude.

Mirzam is 500 light-years from Earth, and its traditional name means "the announcer", referring to its position as the "announcer" of Sirius, as it rises a few minutes before Sirius does. Gamma, also known as Muliphein, is a fainter star of magnitude 4.12, in reality a blue-white bright giant of spectral type B8IIe located 441 light-years from earth. Iota Canis Majoris, lying between Sirius and Gamma, is another star that has been classified as a Beta Cephei variable, varying from magnitude 4.36 to 4.40 over a period of 1.92 hours. It is a remote blue-white supergiant star of spectral type B3Ib, around 46,000 times as luminous as the sun and, at 2500 light-years distant, 300 times further away than Sirius.

Based on parallax measurements from the Hipparcos astrometry satellite, this star is located about from the Earth. It has an apparent visual magnitude of 2.84 and a stellar classification of G5 II. The mass of this star is 3.5 times the mass of the Sun and it is about 240 million years old, which is sufficient time for a star this massive to consume the hydrogen at its core and evolve away from the main sequence, becoming a G-type bright giant. This is a double star system and may be a binary. Using adaptive optics on the AEOS telescope at Haleakala Observatory, the pair was found to be separated by an angle of 2.58 arcseconds at a position angle of 1.4°.

BD+20 2457 is a 10th-magnitude K-type bright giant star located approximately 5,400 light-years away in the constellation of Leo. This star is very metal- poor, containing only 10% as enriched with elements heavier than hydrogen and helium as our sun, almost classifying this as a population II star. On June 10, 2009, two planets were announced to be orbiting the star, with minimum masses 21.4 and 12.5 times the mass of Jupiter and orbital periods of 380 and 622 days for the inner and outer planets, respectively. A dynamical analysis reveals that the proposed system is unstable on astronomically-short timescales and so the suggested planetary configuration is unlikely to be correct: further data is needed to determine a physically-plausible explanation for the radial velocity variations.

Both components are themselves close binaries which can be seen with telescopes to consist of A- and F-type stars, and a faint star was recently found to orbit component C as well, for a total of five stars. In contrast to Zeta and Epsilon Lyrae, Delta Lyrae is an optical double, with the two stars simply lying along the same line of sight east of Zeta. The brighter and closer of the two, Delta2 Lyrae, is a 4th-magnitude red bright giant that varies semiregularly by around 0.2 magnitudes with a dominant period of 79 days, while the fainter Delta1 Lyrae is a spectroscopic binary consisting of a B-type primary and an unknown secondary. Both systems, however, have very similar radial velocities, and are the two brightest members of a sparse open cluster known as the Delta Lyrae cluster.

The Eta Pegasi system consists of a pair of stars in a binary orbit with a period of 813 days and an eccentricity of 0.183. The primary component is a bright giant star with a stellar classification of G2 II and about three and a half times the mass of the Sun. The interferometry-measured angular diameter of this star, after correcting for limb darkening, is , which, at its estimated distance, equates to a physical radius of more than 24 times the radius of the Sun. It is radiating 331 times the luminosity of the Sun from its expanded outer envelope at an effective temperature of 4,970 K. The rotation rate of the star slowed as it expanded, so it has a projected rotational velocity of 1.7 km s−1 with an estimated rotation period of 818 days.

The spectrum of this star matches a stellar classification of G8 II-III, with the luminosity class notation 'II-III' indicating it shows some traits of both a giant star and a bright giant. At this evolutionary stage, the atmosphere has expanded to almost thirteen times the radius of the Sun and the outer envelope has an effective temperature of 5,196 K. X-ray emission has been detected from this star, with an estimated luminosity of . Alpha Reticuli has a 12th-magnitude visual companion, CCDM J04144-6228B, at an angular separation of 48 arcseconds away along a position angle of 355°. Since the two stars share a common proper motion across the celestial sphere, it is possible that Alpha Reticuli, rather than being solitary, may instead be the primary component of a binary star system with an orbital period of, at least, 60,000 years.