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List Of Novae In The Milky Way Galaxy
This is a partial list of novae in the Milky Way galaxy that have been discovered and recorded since 1891. Novae are stars that undergo dramatic explosions, but unlike supernovae, these do not result in the destruction of the original star. The likely rate of novae in the Milky Way is about 40 per year,Prialnik, Dina. "Novae", pp. 1846-56, in Paul Murdin, ed. ''Encyclopedia of Astronomy and Astrophysics.'' London: Institute of Physics Publishing Ltd and Nature Publishing Group, 2001. but of these only about 10 per year are discovered by observers as of the 2000s (decade).CBAT List of Novae in the Milky Way discovered since 1612 This list attempts to include only the brighter or more notable novae. The |
Nova
A nova (plural novae or novas) is a transient astronomical event that causes the sudden appearance of a bright, apparently "new" star (hence the name "nova", which is Latin for "new") that slowly fades over weeks or months. Causes of the dramatic appearance of a nova vary, depending on the circumstances of the two progenitor stars. All observed novae involve white dwarfs in close binary systems. The main sub-classes of novae are classical novae, recurrent novae (RNe), and dwarf novae. They are all considered to be cataclysmic variable stars. Classical nova eruptions are the most common type. They are likely created in a close binary star system consisting of a white dwarf and either a main sequence, subgiant, or red giant star. When the orbital period falls in the range of several days to one day, the white dwarf is close enough to its companion star to start drawing accreted matter onto the surface of the white dwarf, which creates a dense but shallow atmosphere. This atmosphe ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
U Leonis
U or u, is the twenty-first and sixth-to-last letter and fifth vowel letter of the Latin alphabet, used in the modern English alphabet, the alphabets of other western European languages and others worldwide. Its name in English is ''u'' (pronounced ), plural ''ues''. History U derives from the Semitic waw, as does F, and later, Y, W, and V. Its oldest ancestor goes to Egyptian hieroglyphics, and is probably from a hieroglyph of a mace or fowl, representing the sound Voiced_labiodental_fricative.html" ;"title="nowiki/> vor the sound [Voiced labial–velar approximant">w">Voiced labiodental fricative">vor the sound [Voiced labial–velar approximant">w This was borrowed to Phoenician, where it represented the sound [w], and seldom the vowel [Close back rounded vowel, u]. In Greek language, Greek, two letters were adapted from the Phoenician waw. The letter was adapted, but split in two, with the Digamma, first one of the same name (Ϝ) being adapted to represent w">now ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
DM Geminorum
DM Geminorum also known as Nova Geminorum 1903 was a nova which erupted in the constellation Gemini in 1903. It was discovered by Herbert Hall Turner at the Greenwich Observatory on a Carte du Ciel photographic plate taken on 16 March 1903. Post-discovery examination of earlier photographs of the region taken at the Harvard College Observatory showed that the star was fainter than apparent magnitude 9 on 2 March 1903, and magnitude 5.1 on 6 March 1903, making it visible to the naked eye at that time. It had a conspicuous red color due to strong Hα line emission. By 1 April 1903 it had faded to magnitude 8.5. By 1989 it had reached visual magnitude 17.38. DM Geminorum faded from peak brightness by 2 magnitudes in just 6 days, making it a "very fast nova". All novae are binary stars, with a "donor" star orbiting a white dwarf. The two stars are so close together that matter is transferred from the donor to the white dwarf. High speed photometry done with the 1.2 met ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
GK Persei
GK Persei (also Nova Persei 1901) was a bright nova first observed on Earth in 1901. It was discovered by Thomas David Anderson, an Edinburgh clergyman, at 02:40 UT on 22 February 1901 when it was at magnitude 2.7. It reached a maximum magnitude of 0.2, the brightest nova of modern times until Nova Aquilae 1918. After fading into obscurity at about magnitude 12 to 13 during the early 20th century, GK Persei began displaying infrequent outbursts of 2 to 3 magnitudes (about 7 to 15 times quiescent brightness). Since about 1980, these outbursts have become quite regular, typically lasting about two months and occurring about every three years. Thus, GK Persei seems to have changed from a classical nova like Nova Aquilae 1918 to something resembling a typical dwarf nova-type cataclysmic variable star. Surrounding GK Persei is the Firework nebula, a nova remnant first detected in 1902 consisting of an expanding cloud of gas and dust bubbles moving up to 1200 km/s. GK Pe ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
V606 Aquilae
V606 Aquilae was a nova, which lit up in the constellation Aquila in 1899. The brightest reported magnitude for this nova was apparent magnitude 5.5, making it a naked eye object. It was discovered by Williamina Fleming on a photographic plate (one of the Henry Draper Memorial Photographs) taken on 21 April 1899 at the Harvard College Observatory. On the discovery plate, its photographic magnitude was later determined to be 6.75. It was not seen on the plate taken on 1 November 1898, and there were no reported observations of the region around the star during the 171 day interval before Fleming's discovery, so it is possible that the actual maximum of the event was missed. By 27 October 1899 it had faded to 10th magnitude, and on 9 July 1900 Oliver Wendell reported its brightness to be between magnitude 11.5 and 12.0. V606 Aquilae is classified as a "fast nova", because its faded by at least 3 magnitudes in about 65 days. The light curve showed a steep decline, foll ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
V1059 Sagittarii
V1059 Sagittarii (also called Nova Sagittarii 1898) was a nova, which lit up in 1898 in the constellation Sagittarius. The star reached apparent magnitude 4.5, making it easily visible to the naked eye. It was discovered on 8 March 1898, by Williamina Fleming on a photographic plate taken at the Harvard College Observatory. The discovery plate was an objective prism plate, part of the Henry Draper Memorial Photographs, and Ms Fleming identified it as a nova based on its spectral characteristics. The astronomical literature contains a variety of values for V1059 Sagittarii's peak brightness. Özdönmez ''et al.'' list the peak magnitude as 2.0 (visual), while Downes ''et al.'' report a much fainter value of magnitude 4.9 (photographic). Novae are usually classified as "fast" or "slow" based on the time it takes the star to drop from peak brightness by more than 3 magnitudes (T3), but for this nova the decline from maximum was poorly observed, and no T3 value has been report ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
T Aurigae
T Aurigae (or Nova Aurigae 1891) was a nova, which lit up in the constellation Auriga in 1891. Thomas David Anderson, an amateur astronomer in Edinburgh, reported that he was "almost certain" he saw the nova at 02:00 UT on 24 January 1892, when it was slightly brighter than χ Aurigae (apparent magnitude 4.74). He mistook the star for 26 Aurigae, although he noted to himself that it seemed brighter than he remembered it being. He saw it twice more during the following week. On 31 January 1892 he realized his mistake, and wrote a note to Ralph Copeland (the Astronomer Royal of Scotland) reporting his discovery. Professor Copeland immediately reported the discovery via telegram to William Huggins, who made the first spectroscopic observations of T Aurigae on 2 February 1892, when the star was a magnitude 4.5 object. T Aurigae was the first nova to be observed spectroscopically. Strope and Schaefer report that the peak brightness of T Aurigae was magnitude 4.5, ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
V Persei
V Persei, also known as Nova Persei 1887 was discovered by Williamina Fleming on a Harvard College Observatory objective-prism photograph taken on 3 November 1887. It is believed to be the first nova whose spectrum was recorded. The nova had an apparent magnitude of 9.2 at the time of discovery. Judging from the consistency of the nova's brightness after discovery, and details of the spectral lines seen, McLaughlin estimated that the nova was five or six months past peak brightness at the time of its discovery, and at its peak it was almost certainly at least as bright as 4th magnitude. So V Persei was probably visible to the naked eye, though there is no record that anyone actually noticed it when that was possible. It is currently an 18th magnitude object. All novae are binary stars, with a "donor" star orbiting so close to a white dwarf companion that matter is transferred from the donor to the white dwarf. Because the stars are so close together, novae are ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
AB Boötis
AB Boötis, also known as Nova Boötis 1877 and occasionally Nova Comae Berenices 1877, is an object that may have undergone a nova outburst in 1877. It was discovered by Friedrich Schwab at Technische Universität Ilmenau in 1877. He reported observing the star as a 5th magnitude object, visible to the naked eye, on 14 nights during the period from 30 May 1877 through 14 July 1877. The star was lost, and despite several searches in subsequent years, no other 19th century observations of the nova were reported. Downes ''et al.'' estimate that Schwab's reported coordinates for the star may have had a precision no better than 1/2 degree. In 1971, A. Sh. Khatisov suggested that the star Schwab saw was BD +21°2606 (whose visual magnitude is 10.64 in the Tycho-2 Catalogue, roughly 100 times fainter than the object Schwab reported), but that identification may be incorrect. In 1988 Downes and Szkody imaged the area around AB Boötis' reported position, to try to identify the nov ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Q Cygni
Q Cygni (Q Cyg), is a star located in the constellation Cygnus. It is also known as Nova Cygni 1876, and has the designation NGC 7114, and HR 8296. Nova Cygni is located in the northwestern portion of Cygnus along the border with Lacerta. One of the earliest novae recorded, Q Cygni was discovered by astronomer Johann Friedrich Julius Schmidt on November 24, 1876. The star had undergone a nova, brightening to about 3rd magnitude and remaining as bright for four days. The system is termed a cataclysmic variable, composed of a white dwarf in close orbit with another star that orbit each other every 10 hours. The white dwarf is surrounded by an accretion disc, which blazes much brighter than the star it circles. The system has been estimated to be 740 ± 11 parsecs distant. The secondary star has been estimated to be around 0.6 times as massive as the Sun, making it an orange dwarf of spectral type K5. Also known as a donor star, the secondary supplies mass to the white d ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
T Coronae Borealis
T Coronae Borealis (''T CrB''), is a recurring nova in the constellation Corona Borealis. It was first discovered in outburst in 1866 by John Birmingham, although it had been observed earlier as a 10th magnitude star. Description T CrB normally has a magnitude of about 10, which is near the limit of typical binoculars. It has been seen to outburst twice, reaching magnitude 2.0 on May 12, 1866 and magnitude 3.0 on February 9, 1946, although a more recent paper shows the 1866 outburst with a possible peak range of magnitude 2.5 ± 0.5. Even when at peak magnitude of 2.5, this recurrent nova is dimmer than about 120 stars in the night sky. It is sometimes nicknamed the ''Blaze Star''. 34. Unusual Stellar Spectra III: two emission-line stars ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
U Scorpii
U Scorpii (''U Sco'') is a recurrent nova system; one of 10 known recurring novae in the Milky Way galaxy. Located near the northern edge of the constellation Scorpius it normally has a magnitude of 18, but reaches a magnitude of about 8 during outbursts. Outbursts have been observed in 1863, 1906, 1936, 1979, 1987, 1999, 2010, and 2022. The 2010 outburst was predicted to occur April 2009 ± 1.0 year, based on observations during quiescence following the 1999 outburst. The U Sco 2010 eruption faded by 1 magnitude in 1 day, and by 4 magnitudes in 6 days. By February 6 it was dimmer than magnitude 13. Between February 10–19, it was flickering around magnitude 14. The eruption ended on day 64, which is the fastest observed decline to quiescence of recurring nova. This eruption of U Sco is now the best-observed nova event with 22,000 magnitudes already accumulated. Astronomers have predicted that another eruption of U Sco will occur in 2020±2. This prediction was correct; ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
