V392 Persei

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V392 Persei
Location of V392 Persei (circled)
Observation data
Epoch J2000.0      Equinox J2000.0
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]
Distance
4161+2345
−440[5] pc
Absolute magnitude (MV)−10.1 (max)[6]
V392 Per, Gaia DR2 254361745823908736, 2MASS J04432138+4721257[7]
Database references
SIMBADdata

V392 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.

Dwarf nova

A U Geminorum-type variable star or dwarf nova is a type of

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

Nova eruption

AAVSO
data

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

blueshifted by a velocity of 2,680 km/s, which would be the expansion velocity from the nova explosion.[9]

Observations with

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

Gaia parallax.[6]

Gallery

See also

References

  1. ^
    Bibcode:2009yCat....102025S
    .
  2. ^
    Bibcode:2006SASS...25...47W
    .
  3. ^
    doi:10.1086/313380
    .
  4. ^
    doi:10.1051/0004-6361/201833051
    .
  5. S2CID 118925493
    .
  6. ^
    S2CID 119486187
    .
  7. ^ "V392 Per". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-08-25.
  8. ^ 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.
  9. ^ 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.
  10. ^ 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.
  11. ^ R. Konyves-Toth; B. Csak; A. Pal; J. Vinko. "Optical Photometry of the Nova Outburst TCP J04432130+4721280 (V392 Per)". Retrieved 2018-05-02.
  12. S2CID 235632263
    .
  13. ^ "Nova over Supernova". www.eso.org. Retrieved 7 May 2018.

External links

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