But Russian astronomer Stanislav Short of the telescope astronomical station Tau has said the comet poses no danger and that such objects pass by our planet all the time without incident.
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The CERGA Observatory (; obs. code: 010) was a scientific department and astronomical station of the Côte d'Azur Observatory in southern France, where several asteroids were discovered during 1984–1993.
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This team used an air shower array at Harvard University's Agassiz Astronomical Station to observe air showers created by cosmic rays using ground-based liquid scintillator detectors. The analysis techniques Rossi's group developed laid the groundwork for the analysis of data from future arrays.
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Félix Aguilar Observatory ( ; OAFA) is an astronomical observatory. It was established in 1953, in San Juan Province, Argentina. In 1974, it was renamed to Carlos Ulrrico Cesco Astronomical Station ( ; EACUC). Its primary observing facility is located El Leoncito National Park in the west of San Juan Province.
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In December 2006, a rotational lightcurve of Leocadia was obtained from photometric observations by Italian amateur astronomers Roberto Crippa and Federico Manzini at the Sozzago Astronomical Station . Lightcurve analysis gave a rotation period of hours with a brightness amplitude of magnitude (), which is indicative of a rather spherical, non-irregular shape.
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2013 Tucapel, provisional designation , is an eccentric Florian asteroid from the inner regions of the asteroid belt, approximately 11 kilometers in diameter. It was discovered on 22 October 1971, by the University of Chile's National Astronomical Observatory at Cerro El Roble Astronomical Station. It was named for one of the indigenous Mapuche chiefs.
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Lightcurve-based 3D-model of Bodea In September 2006, a rotational lightcurve of Bodea was obtained from photometric observations by Italian astronomers Roberto Crippa and Federico Manzini at the Sozzago Astronomical Station . Lightcurve analysis gave a well defined rotation period of hours with a relatively high brightness amplitude of magnitude (), which is indicative of an elongated, irregular shape.
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Additional period determinations: 6+ hours by Jean-Gabriel Bosch at the Collonges Observatory (), 6.145 hours at the Catania and Pino Torinese observatories in 2000 (), 8.3945 hours by René Roy in 2016 (), 8.397 hours by V. G. Chiorny in 2003 and 2007 (), and 8.4 hours by Roberto Crippa and Federico Manzini at the Sozzago Astronomical Station in 2010 ().
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The observatory in Kryoneri The Kryoneri Astronomical Station observatory was built in 1974–75 at a height of 1000 meters. It has the second biggest telescope in Greece after the Chelmos Observatory. Its catoptric lens is 122 cm diameter. Located 4 km southwest of the village is the monastery of the Assumption of the Theotokos Lechova.
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They also built the Kislovodsk Mountain Astronomical Station and a laboratory in Blagoveshchensk. The observatory organized many expeditions for determining differences of longitudes, observing passages of Venus and solar eclipses, and studying astroclimate. In 1962, the Observatory sent an expedition to Chile to observe stars in the southern skies.Frank Kelly Edmondson AURA and its US national observatories pp.
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In August 2012, a rotational lightcurve of David Hughes was obtained from photometric observations by Italian amateur astronomers Roberto Crippa and Federico Manzini at the Sozzago Astronomical Station . Lightcurve analysis gave a rotation period of at least 24 hours with a brightness amplitude of 0.25 magnitude (). Most asteroids have a period shorter than 20 hours (also see List of slow rotators).
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Astro Glacier () is a glacier in Antarctica, between the Turner Hills and Tricorn Peak in the Miller Range, flowing northeast into the Marsh Glacier. It was seen by the northern party of the New Zealand Geological Survey Antarctic Expedition (1961-62) and so named because an astronomical station was set up on the bluff at the mouth of the glacier in December 1961.
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In December 2005, a rotational lightcurve of Romilda was obtained from photometric observations over seven nights by Walter Cooney at the Blackberry Observatory in Louisiana. Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude (). In January 2006, Italian astronomers Roberto Crippa and Federico Manzini at the Sozzago Astronomical Station determined a nearly identical period of hours with an amplitude of magnitude ().
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Observations performed by Brian Warner at the Palmer Divide Observatory in Colorado Springs, Colorado, during 2007 produced a lightcurve with a period of 10.080 ± 0.005 hours and a brightness range of 0.17 ± 0.02 in magnitude (). Another lightcurve obtained by Italian amateur astronomers Roberto Crippa and Federico Manzini at the Sozzago Astronomical Station () gave a period of 9.0127 hours with an amplitude of 0.17 magnitude ().
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In 1808, von Zach was in Marseille where he observed and explained the phenomenon of the Canigou mountain in eastern Pyrénées which can be seen twice a year from there, 250 km away, by refraction of light. Asteroid 999 Zachia and the crater Zach on the Moon are named after him, while asteroid 64 Angelina is named after an astronomical station he set up near Marseille.
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Angelina was discovered on March 4, 1861, by a prolific comet discoverer, E. W. Tempel, observing from Marseilles, France. It was the first of his five asteroid discoveries. The naming of Angelina caused some controversy. It was chosen by Benjamin Valz, director of the Marseilles Observatory, in honour of the astronomical station of that name operated by Baron Franz Xaver von Zach on the mountains above the city.
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In November 2005, a rotational lightcurve of La Paz was obtained from photometric observations by French amateur astronomer René Roy. Lightcurve analysis gave a well-defined rotation period of 8.998 hours with a brightness amplitude of 0.14 magnitude (). In March 2007, a concurring period of 9.002 hours and an amplitude of 0.14 magnitude () was obtained by astronomers Roberto Crippa and Federico Manzini at the Sozzago Astronomical Station in Italy ().
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In August 2006, a rotational lightcurve of Athene was obtained from photometric observations by Roberto Crippa and Federico Manzini at the Sozzago Astronomical Station , Italy, and by Jean-Gabriel Bosch at the Collonges Observatory , France. Lightcurve analysis gave a rotation period of hours with a high brightness variation of magnitude, indicative of a non- spherical, elongated shape (). In September 2010, French amateur astronomer René Roy measured a similar period of hours and an amplitude of ().
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3361 Orpheus (1982 HR) is an Apollo asteroid that was discovered on 24 April 1982 by Carlos Torres at Cerro El Roble Astronomical Station. Its eccentric orbit crosses that of Mars and Earth, and approaches Venus as well. From 1900 to 2100 it passes closer than 30 Gm to Venus 11, Earth 33, and Mars 14 times. It passed by Earth at a distance of about 40 lunar distances on 7 December 2013.
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In December 2010, a rotational lightcurve of Ajax was obtained from photometric observations taken by Robert Stephens at the Goat Mountain Astronomical Research Station in California. Lightcurve analysis gave a rotation period of 29.38 hours with a brightness variation of 0.30 magnitude (), superseding fragmentary photometric measurements by Richard P. Binzel (1988), and by Roberto Crippa and Federico Manzini (2009) at the Sozzago Astronomical Station , which gave a period of 28.4 and 34 hours, respectively ().
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In September 2017, a rotational lightcurve of Swetlana was obtained from photometric observations by Thomas A. Polakis at the Command Module Observatory in Arizona. Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of magnitude (). The result supersedes an observations by Italian amateur astronomers Roberto Crippa and Federico Manzini at the Sozzago Astronomical Station from September 2006, which tentatively determined a period of more than 20 hours and an amplitude of magnitude ().
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In October 1999, a first rotational lightcurve of Pamela was obtained from photometric observations by Brian Warner at his Palmer Divide Observatory in Colorado, United States. Lightcurve analysis gave a rotation period of 26.017 hours with a brightness amplitude of 0.49 magnitude (). Other lightcurves were taken by the Spanish amateur group OBAS in 2015 (), as well as by René Roy and Stéphane Charbonnel in France, and Roberto Crippa and Federico Manzini at Sozzago Astronomical Station () in Piedmont, Italy, between 2005 and 2010 ().
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In February 2005, Federico Manzini at the Sozzago Astronomical Station in Italy obtained the first rotational lightcurve of '. It gave a tentative rotation period of 16.04 hours with a brightness amplitude of 0.22 based on three nights of observation magnitude (). In June 2006, photometric observations over eight nights were made by Italian astronomer Stefano Mottola at the Calar Alto Observatory in Spain. Lightcurve analysis gave a rotation period of hours with a brightness amplitude of 0.20 magnitude (), superseding Manzini's previous result.
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In January 2006, a rotational lightcurve of Yukitsuna was obtained from photometric observations by Federico Manzini at the Sozzago Astronomical Station in Italy. Lightcurve analysis gave a rotation period of 19.2 hours with a brightness variation of 0.8 magnitude (). In September 2008, a more refined period of 19.04 hours and an amplitude of 0.80 magnitude was measured at the Oakley Southern Sky Observatory and Oakley Observatory (). The high brightness variation of 0.8 magnitude is indicative for an elongated, non-spherical shape.
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A first rotational lightcurve of Memnon was obtained by American astronomer Richard Binzel in the early 1980s. It gave a rotation period of 7.5 hours with a brightness variation of 0.24 magnitude (). In February 2005, a fragmentary lightcurve by Italian astronomer Federico Manzini at the Sozzago Astronomical Station gave a period of 7 hours (). The so-far best rated lightcurve was obtained in November 1990, by Italian astronomer Stefano Mottola using the ESO 1-metre telescope at the La Silla Observatory in northern Chile.
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The institute has mountain observatories at Skalnaté Pleso, Lomnický štít and a theoretical department in Bratislava (founded in 1955), which is a statewide coordinating body for research of interplanetary matter. Moreover, it runs several full-sky photographic chambers (bolide cameras) which are part of European bolide network. The astronomical observatory at Skalnaté Pleso (1783 m) was founded in 1943. It is equipped with a 61 cm astrometrical and photometric reflector with a CCD camera and a 60 cm photometric reflector. The astronomical station on Lomnický štít (2632 m) has been active since 1960.
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In March 2015, a rotational lightcurve of Bredichina was obtained from photometric observations by Spanish astronomers Alfonso Carreño , Amadeo Aznar , Enrique Arce , Pedro Brines , and Juan Lozano . Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude (). Previously, in August 2008, Argentine astronomer Ricardo Gil-Hutton derived period of hours with an amplitude of magnitude (). Tentative measurements were also made by Italian Nicola Cornero and Federico Manzini at the Sozzago Astronomical Station in May 2010, which gave a period of hours with an amplitude of magnitude ().
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Vergara studied physical sciences and astronomy, at a time when both fields were inaccessible for women. She was part of the first generation of students of the Astronomy Department founded by Dr. Cernuschi in the University of the Republic's . In 1952, she was one of the founders of the Association of Astronomy Aficionados. She was secretary of the Uruguayan Antarctic Institute. On 18 July 1968, Chilean astronomers Carlos Torres and S. Cofré discovered, at the Cerro El Roble Astronomical Station in Chile, a new main belt asteroid that was provisionally designated 1968 OA1.
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In December 2009, a rotational lightcurve of Petunia was obtained from photometric observations by Robert Stephens at Santana Observatory and Goat Mountain Astronomical Research Station in California. Lightcurve analysis gave a long rotation period of hours with a brightness variation of magnitude (). Astronomers at the Palomar Transient Factory in California measured a period of hours and an amplitude of 0.30 magnitude in August 2013 (), while observations by Italian amateur astronomers Roberto Crippa and Federico Manzini at the Sozzago Astronomical Station in April 2006 were of poor quality (). A modeled lightcurve using photometric data from the Lowell Photometric Database was published in 2016.
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In November 2013, a rotational lightcurve of Schwassmannia was obtained from photometric observations by astronomers Vladimir Benishek at Sopot Astronomical Observatory , Serbia, American Frederick Pilcher at his Organ Mesa Observatory , New Mexico, and Luis Martinez at Lenomiya Observatory at Casa Grande in Arizona. Lightcurve analysis gave a well-defined rotation period of hours with a brightness amplitude of magnitude (). Alternative observations with a lower rated quality by Robert Stephens at the Center for Solar System Studies in September 2013 gave a period of hours (). The results supersede an earlier, tentative observation by Italian Federico Manzini at the Sozzago Astronomical Station from October 2004, with an incorrect period 4.5 hours ().
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In April 2007, a rotational lightcurve of Troilus was obtained from photometric observations by Lawrence Molnar at the Calvin-Rehoboth Robotic Observatory in New Mexico. Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude (). While not being a slow rotator, Troilus has a significantly longer period than most asteroids, and one of longest of all larger Jupiter trojans. The period also supersedes previous observations made by Linda French with the 0.9-meter SMARTS telescope at Cerro Tololo in the 1980s and by Federico Manzini at the Sozzago Astronomical Station , which gave a period of 24 and 63.8 hours, respectively ().
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During five nights in December 2017, a rotational lightcurve of Angelica was obtained from photometric observations by Tom Polakis at the Command Module Observatory in Tempe, Arizona. Lightcurve analysis gave a rotation period of hours with a very low brightness variation of magnitude (), which is indicative of regular, spherical shape. Another observation from January 2018, by Brigitte Montminy and Katherine McDonald at Minnetonka High School, and Russell Durkee at the Shed of Science Observatory in Minnetonka, Minnesota, determined a concurring period of hours with an amplitude of magnitude (). Federico Manzini at the Sozzago Astronomical Station obtained the object's first lightcurve in December 2006, measuring a period of hours and an amplitude magnitude ().
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In September 2007, a rotational lightcurve of Jürgenstock was obtained from photometric observations by Federico Manzini at the Sozzago Astronomical Station in Italy. Lightcurve analysis gave a rotation period of hours with a brightness variation of 0.11 magnitude, indicative of a spherical rather than elongated shape (). In July 2014, a similar period determination of hours and an amplitude of 0.10 magnitude was made by Brian Warner at the Palmer Divide Station in California (). While Manzini and/or Raoul Behrend suspected it to be an asynchronous binary asteroid with a minor-planet moon in its orbit, Warner did not mention any anomalies in the lightcurve, and the Lightcurve Data Base does not flag the body as a potential binary system.
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Newall was a keen astronomer, and he commissioned Thomas Cooke to build a telescope for his private observatory at Ferndene, his Gateshead residence. For many years, the 25 inch refracting telescope was the largest in the world, and it was gifted to the Cambridge Observatory after his death in 1889. By the end of the 1950s, the telescope had fallen into disuse, and in 1958 it was donated to the National Observatory of Athens and it was placed at the Penteli Astronomical Station, just north of the city of Athens. He was elected a fellow of the Royal Astronomical Society in 1864, of the Royal Society in 1875, and became in 1879 a member of the Institute of Mechanical Engineers.
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Lightcurve-based 3D-model of Kovacia In February 2008, a rotational lightcurve of Kovacia was obtained from photometric observations by a collaboration of French and Italian amateur astronomers including René Roy, Silvano Casulli, François Colas, Arnaud Leroy, Federico Manzini, Christophe Demeautis and Jean-François Coliac. Lightcurve analysis gave a well-defined rotation period of hours with a high brightness variation of magnitude, indicative of a non-spherical, elongated shape (). The result supersedes a previous observation by Roberto Crippa and Federico Manzini at the Sozzago Astronomical Station from November 2006, that determined a lower limit of 6 hours (). Due to observed mutual occultation and eclipsing events, the collaboration of astronomers strongly suspect Kovacia to be a binary asteroid with a satellite orbiting it every days.
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