Nova Persei 2018
Epoch J2000.0 Equinox J2000.0
|Right ascension||04h 43m 21.37s|
|Declination||+47° 21′ 25.9″|
|Apparent magnitude (V)||6.3 - 16.9|
|B−V color index||+1.0|
|V−R color index||+0.9|
|Variable type||dwarf nova & nova|
|Proper motion (μ)|| RA: 0.193 mas/yr |
Dec.: −1.749 mas/yr
|Parallax (π)||0.2573 ± 0.0516 mas|
|Absolute magnitude (MV)||−10.1 (max)|
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. 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. Its spectrum in the quiescent state has been studied and only the cool star is detected. The spectrum shows emission lines of hydrogen-alpha (Hα) and both neutral and ionised helium. The brightest recorded observations is at magnitude 5.6.
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 Hα and FeII emission lines with P Cygni profiles. The absorption core is blueshifted by a velocity of 2,680 km/s, which would be the expansion velocity from the nova explosion.
Observations with Fermi-LAT on April 30 show a strong gamma-ray source at the coordinates of the nova. 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.
V392 Persei is the southern of a pair of stars separated by 8.5".
The symbiotic pair are unresolved 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 ly suggested by its Gaia parallax.
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- 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...2b..24D. doi:10.3847/2515-5172/aac26c.
- "V392 Per". SIMBAD. Centre de données 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.
- "Nova over Supernova". www.eso.org. Retrieved 7 May 2018.
- Dwarf Nova V392 Persei Goes Big — It’s Now Binocular Bright
- How A Dwarf Nova Hit The Big Time May 2, 2018
- Nova in Perseus
- V392 Per in outburst, showing spectra of the nova in outburst and previously