[{"@context":"http:\/\/schema.org\/","@type":"BlogPosting","@id":"https:\/\/wiki.edu.vn\/en\/wiki43\/v392-persei-wikipedia\/#BlogPosting","mainEntityOfPage":"https:\/\/wiki.edu.vn\/en\/wiki43\/v392-persei-wikipedia\/","headline":"V392 Persei – Wikipedia","name":"V392 Persei – Wikipedia","description":"From Wikipedia, the free encyclopedia Nova in the constellation Perseus V392 Persei, also known as Nova Persei 2018, is a","datePublished":"2021-05-21","dateModified":"2021-05-21","author":{"@type":"Person","@id":"https:\/\/wiki.edu.vn\/en\/wiki43\/author\/lordneo\/#Person","name":"lordneo","url":"https:\/\/wiki.edu.vn\/en\/wiki43\/author\/lordneo\/","image":{"@type":"ImageObject","@id":"https:\/\/secure.gravatar.com\/avatar\/c9645c498c9701c88b89b8537773dd7c?s=96&d=mm&r=g","url":"https:\/\/secure.gravatar.com\/avatar\/c9645c498c9701c88b89b8537773dd7c?s=96&d=mm&r=g","height":96,"width":96}},"publisher":{"@type":"Organization","name":"Enzyklop\u00e4die","logo":{"@type":"ImageObject","@id":"https:\/\/wiki.edu.vn\/wiki4\/wp-content\/uploads\/2023\/08\/download.jpg","url":"https:\/\/wiki.edu.vn\/wiki4\/wp-content\/uploads\/2023\/08\/download.jpg","width":600,"height":60}},"image":{"@type":"ImageObject","@id":"https:\/\/upload.wikimedia.org\/wikipedia\/commons\/thumb\/6\/64\/V392PerLightCurve.png\/220px-V392PerLightCurve.png","url":"https:\/\/upload.wikimedia.org\/wikipedia\/commons\/thumb\/6\/64\/V392PerLightCurve.png\/220px-V392PerLightCurve.png","height":"137","width":"220"},"url":"https:\/\/wiki.edu.vn\/en\/wiki43\/v392-persei-wikipedia\/","wordCount":3265,"articleBody":"From Wikipedia, the free encyclopediaNova in the constellation PerseusV392 Persei, also known as Nova Persei 2018, is a bright nova in the constellation Perseus discovered on April 29, 2018.  It was previously known as a dwarf nova.Table of ContentsDwarf nova[edit]Nova eruption[edit]Gallery[edit]See also[edit]References[edit]External links[edit]Dwarf nova[edit]A U Geminorum-type variable star or dwarf nova is a type of cataclysmic variable star consisting of a close binary star system in which one of the components is a white dwarf that accretes matter from a cool main sequence or subgiant companion.[8]  V392 Persei was discovered in 1970 and received its variable star designation a year later.  It is normally visual magnitude 17.4 and experiences outbursts of 2-3 magnitudes.[1]  Its spectrum in the quiescent state has been studied and only the cool star is detected.  The spectrum shows emission lines of hydrogen-alpha (H\u03b1) and both neutral and ionised helium.[3]  The brightest recorded observations is at magnitude 5.6.[6]Nova eruption[edit]  On April 29, 2018 it was discovered by Yuji Nakamura to be extremely bright, and it was spectroscopically confirmed as a nova outburst with magnitude 6.2 on April 30.  The spectrum includes broad H\u03b1 and FeII emission lines with P Cygni profiles.  The absorption core is blueshifted by a velocity of 2,680\u00a0km\/s, which would be the expansion velocity from the nova explosion.[9]Observations with Fermi-LAT on April 30 show a strong gamma-ray source at the coordinates of the nova.[10]Photometry of the nova from Konkoly Observatory on May 1, 2018 give apparent magnitudes of 7.38 in the V band and 8.22 in the B band, suggesting it is already declining.[11]V392 Persei is the southern of a pair of stars separated by 8.5″.[2]The symbiotic pair are unresolved, with an orbital period of only 3.21997 days,[12] and the nature of the cool component is unclear.  The spectral energy distribution is inconsistent with a bright giant star but it could be less luminous red clump giant or subgiant.  If the cool component was a main sequence red dwarf as expected for a dwarf nova, then the system would need to be closer than the 13,000\u00a0ly suggested by its Gaia parallax.[6]Gallery[edit]See also[edit]References[edit]^ a b c d Samus, N. N.; Durlevich, O. V.;  et\u00a0al. (2009). “VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)”. VizieR On-line Data Catalog: B\/GCVS. Originally Published in: 2009yCat….102025S. 1. Bibcode:2009yCat….102025S.^ a b Watson, C. L. (2006). “The International Variable Star Index (VSX)”. The Society for Astronomical Sciences 25th Annual Symposium on Telescope Science. Held May 23\u201325. 25: 47. Bibcode:2006SASS…25…47W.^ a b c Liu, Wu; Hu, J. Y (2000). “Spectroscopic Confirmation of Northern and Equatorial Cataclysmic Variables. III. 32 Poorly Known Objects”. The Astrophysical Journal Supplement Series. 128 (1): 387\u2013401. Bibcode:2000ApJS..128..387L. doi:10.1086\/313380.^ a b c Brown, A. G. A.;  et\u00a0al. (Gaia collaboration) (August 2018). “Gaia Data Release 2: Summary of the contents and survey properties”. Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A…616A…1G. doi:10.1051\/0004-6361\/201833051.^ Schaefer, Bradley E. (2018). “The distances to Novae as seen by Gaia”. Monthly Notices of the Royal Astronomical Society. 481 (3): 3033\u20133051. arXiv:1809.00180. Bibcode:2018MNRAS.481.3033S. doi:10.1093\/mnras\/sty2388. S2CID\u00a0118925493.^ a b c Darnley, M. J; Starrfield, S (2018). “On the Progenitor System of V392 Persei”. Research Notes of the AAS. 2 (2): 24. arXiv:1805.00994. Bibcode:2018RNAAS…2…24D. doi:10.3847\/2515-5172\/aac26c. S2CID\u00a0119486187.^ “V392 Per”. SIMBAD. Centre de donn\u00e9es astronomiques de Strasbourg. Retrieved 2019-08-25.^ N.N. Samus; O.V. Durlevich (February 12, 2009). “GCVS Variability Types and Distribution Statistics of Designated Variable Stars According to their Types of Variability”. Retrieved 2013-02-08.^ R. M. Wagner; D. Terndrup; M. J. Darnley; S. Starrfield; C. E. Woodward; M. Henze. “Optical Spectroscopy of TCP J04432130+4721280 (V392 Per) Confirms a Nova Eruption”. Retrieved 2018-05-02.^ Kwan-Lok Li; Laura Chomiuk; Jay Strader. “Bright gamma-ray emission from TCP J04432130+4721280 (V392 Per) detected by Fermi-LAT”. Retrieved 2018-05-02.^ R. Konyves-Toth; B. Csak; A. Pal; J. Vinko. “Optical Photometry of the Nova Outburst TCP J04432130+4721280 (V392 Per)”. Retrieved 2018-05-02.^ Schaefer, Bradley E. (2021). “Discovery of 13 New Orbital Periods for Classical Novae”. Research Notes of the AAS. 5 (6): 150. arXiv:2106.13907. Bibcode:2021RNAAS…5..150S. doi:10.3847\/2515-5172\/ac0d5b. S2CID\u00a0235632263.^ “Nova over Supernova”. www.eso.org. Retrieved 7 May 2018.External links[edit]"},{"@context":"http:\/\/schema.org\/","@type":"BreadcrumbList","itemListElement":[{"@type":"ListItem","position":1,"item":{"@id":"https:\/\/wiki.edu.vn\/en\/wiki43\/#breadcrumbitem","name":"Enzyklop\u00e4die"}},{"@type":"ListItem","position":2,"item":{"@id":"https:\/\/wiki.edu.vn\/en\/wiki43\/v392-persei-wikipedia\/#breadcrumbitem","name":"V392 Persei – Wikipedia"}}]}]