Astronomy:Nova Persei 2018

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Nova Persei 2018
Perseus IAU.svg
Red circle.svg
Location of V392 Persei (circled)
Observation data
Equinox J2000.0]] (ICRS)
Constellation Perseus
Right ascension  04h 43m 21.37s[1]
Declination +47° 21′ 25.9″[1]
Apparent magnitude (V) 6.3 - 16.9[2]
Characteristics
B−V color index +1.0[3]
V−R color index +0.9[3]
Variable type dwarf nova & nova[1]
Astrometry
Proper motion (μ) RA: 0.193[4] mas/yr
Dec.: −1.749[4] mas/yr
Parallax (π)0.2573 ± 0.0516[4] mas
Distance4161+2345
−440[5] pc
Absolute magnitude (MV)−10.1 (max)[6]
Other designations
AAVSO 0435+47, V392 Per, Gaia DR2 254361745823908736, 2MASS J04432138+4721257[7]
Database references
SIMBADdata

Nova Persei 2018 is a bright nova in the constellation Perseus discovered on April 29, 2018. It was previously known as a dwarf nova with variable star designation V392 Persei.

Dwarf nova

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 (Hα) and both neutral and ionised helium.[3] The brightest recorded observations is at magnitude 5.6.[6]

Nova eruption

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.[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]

System

V392 Persei is the southern of a pair of stars separated by 8.5".[2]

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.[6]

Gallery

  • Dwarf nova V392 Persei over the ESO Supernova Planetarium & Visitor Centre.[12]

  • V392 Persei, 2 May 2018, 22:00 UT. The slightly fainter nearby star is 9th magnitude BD+47°1026. Up is approximately east.

See also

  • List of novae in the Milky Way galaxy

References

  1. ↑ 1.0 1.1 1.2 1.3 Samus, N. N. et al. (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. 
  2. ↑ 2.0 2.1 Watson, C. L. (2006). "The International Variable Star Index (VSX)". The Society for Astronomical Sciences 25th Annual Symposium on Telescope Science. Held May 23–25 25: 47. Bibcode: 2006SASS...25...47W. 
  3. ↑ 3.0 3.1 3.2 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: 387. doi:10.1086/313380. Bibcode: 2000ApJS..128..387L. 
  4. ↑ 4.0 4.1 4.2 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G. 
  5. ↑ Schaefer, Bradley E. (2018). "The distances to Novae as seen by Gaia". Monthly Notices of the Royal Astronomical Society 481 (3): 3033–3051. doi:10.1093/mnras/sty2388. Bibcode: 2018MNRAS.481.3033S. 
  6. ↑ 6.0 6.1 6.2 Darnley, M. J; Starrfield, S (2018). "On the Progenitor System of V392 Persei". Research Notes of the AAS 2 (2): 24. doi:10.3847/2515-5172/aac26c. Bibcode: 2018RNAAS...2b..24D. 
  7. ↑ "V392 Per". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=V392+Per. 
  8. ↑ "GCVS Variability Types and Distribution Statistics of Designated Variable Stars According to their Types of Variability". February 12, 2009. http://www.sai.msu.su/groups/cluster/gcvs/gcvs/iii/vartype.txt. Retrieved 2013-02-08. 
  9. ↑ "Optical Spectroscopy of TCP J04432130+4721280 (V392 Per) Confirms a Nova Eruption". http://www.astronomerstelegram.org/?read=11588. Retrieved 2018-05-02. 
  10. ↑ "Bright gamma-ray emission from TCP J04432130+4721280 (V392 Per) detected by Fermi-LAT". http://www.astronomerstelegram.org/?read=11590. Retrieved 2018-05-02. 
  11. ↑ "Optical Photometry of the Nova Outburst TCP J04432130+4721280 (V392 Per)". http://www.astronomerstelegram.org/?read=11594. Retrieved 2018-05-02. 
  12. ↑ "Nova over Supernova". https://www.eso.org/public/images/potw1819a/. Retrieved 7 May 2018. 

External links




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