From Wikipedia, the free encyclopedia
M31-RV

Light curves for M31-RV, adapted from Boschi and Munari (2004). [1] The red dots show the red band magnitude, and the blue dots show the blue band magnitude.
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Andromeda
Right ascension 00h 43m 02.433s [2]
Declination 41° 12′ 56.17″ [2]
Characteristics
Evolutionary stage M supergiant [1]
Spectral type M0I-M7I [1]
Variable type Luminous Red Nova
Details
Radius2,000 [3]  R
Luminosity900,000 [3] [a]  L
Temperature4,000 [3]  K
Other designations
M31 V1006, M31 V1007, McD 88 1
Database references
SIMBAD data

M31-RV is a possible red cataclysmic variable star located in the Andromeda Galaxy (M31) that experienced an outburst in 1988, which is similar to the outburst V838 Monocerotis experienced in 2002. [3] Such objects have been called luminous red novae or intermediate-luminosity red transients. During the outburst, both V838 Mon and M31-RV reached a maximum absolute visual magnitude of -9.8. [1]

In 2006, the area around M31-RV was observed using the Hubble Space Telescope, but only red giants were seen. Most likely the star either became too dim for Hubble to see, the star is a companion of one of the red giants, or the star is one of the red giants themselves. [2]

M31-RV reached a peak visual magnitude of 17 before fading rapidly and showing dust formation. The most likely explanation states that these outbursts occur during stellar merger events. [4]

See also

Notes

  1. ^ Calculated using the Stefan-Boltzmann Law using the given values for radius and temperature in the reference

References

  1. ^ a b c d Boschi, F.; Munari, U. (2004). "M 31-RV evolution and its alleged multi-outburst pattern". Astronomy and Astrophysics. 418 (3): 869–875. arXiv: astro-ph/0402313. Bibcode: 2004A&A...418..869B. doi: 10.1051/0004-6361:20035716. S2CID  18582562.
  2. ^ a b c Bond, Howard E. (2011). "Hubble Space Telescope Imaging of the Outburst Site of M31 RV. II. No Blue Remnant in Quiescence". The Astrophysical Journal. 737 (1): 17. arXiv: 1105.4595. Bibcode: 2011ApJ...737...17B. doi: 10.1088/0004-637X/737/1/17. S2CID  118561097.
  3. ^ a b c d Evans, A.; Geballe, T. R.; Rushton, M. T.; Smalley, B.; van Loon, J. T.; Eyres, S. P. S.; Tyne, V. H. (2003-08-11). "V838 Mon: an L supergiant?". Monthly Notices of the Royal Astronomical Society. 343 (3): 1054–1056. Bibcode: 2003MNRAS.343.1054E. doi: 10.1046/j.1365-8711.2003.06755.x. ISSN  0035-8711.
  4. ^ Kochanek, C. S.; Adams, Scott M.; Belczynski, Krzysztof (2014). "Stellar mergers are common". Monthly Notices of the Royal Astronomical Society. 443 (2): 1319. arXiv: 1405.1042. Bibcode: 2014MNRAS.443.1319K. doi: 10.1093/mnras/stu1226. S2CID  118617376.


From Wikipedia, the free encyclopedia
M31-RV

Light curves for M31-RV, adapted from Boschi and Munari (2004). [1] The red dots show the red band magnitude, and the blue dots show the blue band magnitude.
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Andromeda
Right ascension 00h 43m 02.433s [2]
Declination 41° 12′ 56.17″ [2]
Characteristics
Evolutionary stage M supergiant [1]
Spectral type M0I-M7I [1]
Variable type Luminous Red Nova
Details
Radius2,000 [3]  R
Luminosity900,000 [3] [a]  L
Temperature4,000 [3]  K
Other designations
M31 V1006, M31 V1007, McD 88 1
Database references
SIMBAD data

M31-RV is a possible red cataclysmic variable star located in the Andromeda Galaxy (M31) that experienced an outburst in 1988, which is similar to the outburst V838 Monocerotis experienced in 2002. [3] Such objects have been called luminous red novae or intermediate-luminosity red transients. During the outburst, both V838 Mon and M31-RV reached a maximum absolute visual magnitude of -9.8. [1]

In 2006, the area around M31-RV was observed using the Hubble Space Telescope, but only red giants were seen. Most likely the star either became too dim for Hubble to see, the star is a companion of one of the red giants, or the star is one of the red giants themselves. [2]

M31-RV reached a peak visual magnitude of 17 before fading rapidly and showing dust formation. The most likely explanation states that these outbursts occur during stellar merger events. [4]

See also

Notes

  1. ^ Calculated using the Stefan-Boltzmann Law using the given values for radius and temperature in the reference

References

  1. ^ a b c d Boschi, F.; Munari, U. (2004). "M 31-RV evolution and its alleged multi-outburst pattern". Astronomy and Astrophysics. 418 (3): 869–875. arXiv: astro-ph/0402313. Bibcode: 2004A&A...418..869B. doi: 10.1051/0004-6361:20035716. S2CID  18582562.
  2. ^ a b c Bond, Howard E. (2011). "Hubble Space Telescope Imaging of the Outburst Site of M31 RV. II. No Blue Remnant in Quiescence". The Astrophysical Journal. 737 (1): 17. arXiv: 1105.4595. Bibcode: 2011ApJ...737...17B. doi: 10.1088/0004-637X/737/1/17. S2CID  118561097.
  3. ^ a b c d Evans, A.; Geballe, T. R.; Rushton, M. T.; Smalley, B.; van Loon, J. T.; Eyres, S. P. S.; Tyne, V. H. (2003-08-11). "V838 Mon: an L supergiant?". Monthly Notices of the Royal Astronomical Society. 343 (3): 1054–1056. Bibcode: 2003MNRAS.343.1054E. doi: 10.1046/j.1365-8711.2003.06755.x. ISSN  0035-8711.
  4. ^ Kochanek, C. S.; Adams, Scott M.; Belczynski, Krzysztof (2014). "Stellar mergers are common". Monthly Notices of the Royal Astronomical Society. 443 (2): 1319. arXiv: 1405.1042. Bibcode: 2014MNRAS.443.1319K. doi: 10.1093/mnras/stu1226. S2CID  118617376.



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