2010ApJ...725..824S


C.D.S. - SIMBAD4 rel 1.7 - 2020.10.19CEST19:02:30

2010ApJ...725..824S - Astrophys. J., 725, 824-830 (2010/December-2)

The red nova-like variable in M31–A blue candidate in quiescence.

SHARA M.M., ZUREK D., PRIALNIK D., YARON O. and KOVETZ A.

Abstract (from CDS):

M31-RV was an extraordinarily luminous (∼106 L) eruptive variable, displaying very cool temperatures (roughly 1000 K) as it faded. While this object's peak luminosity matched or exceeded those of the brightest known classical novae, its red colors and cool spectra were very different from those of classical novae. The photometric behavior of M31-RV (and several other very red novae, i.e., luminous eruptive red variables) has led to several models of this apparently new class of astrophysical object. We list these models, which predict very red eruptions and very red remnants decades after the eruptions. One of the most detailed models is that of "mergebursts." Mergebursts are (hypothetical) mergers of close binary stars, predicted to rival or exceed the brightest classical novae in luminosity, but to be much cooler and redder than classical novae, and to become slowly hotter and bluer as they age. This prediction suggests two stringent and definitive tests of the mergeburst hypothesis. First, there should always be a cool red remnant, and NOT a hot blue remnant at the site of such an outburst. Second, the inflated envelope of a mergeburst event should be slowly contracting; hence, it must display a slowly rising effective temperature. We have searched the location of M31-RV in multiple observatory archives. Our search revealed a luminous, UV-bright object within 0".4 (1.5σ of the astrometric position) of M31-RV in archival WFPC2 images taken 10 years after the outburst. Recent Hubble imagery, 20 years after the outburst, determines that this object is still hot and fading; it remains much too hot to be a mergeburst. Furthermore, the effective temperature of this object is declining, contrary to the prediction for mergebursts. If we have correctly identified M31-RV's remnant, it cannot be a mergeburst–but its behavior is consistent with theoretical nova models which erupt on a low-mass white dwarf. Future Hubble UV and visible images could determine if the M31-RV analogs (in M85 and in M99) are also much more blue than mergeburst theory predicts, and if they, too, are cooling in contradiction to mergeburst theory.

Abstract Copyright:

Journal keyword(s): binaries: close - galaxies: stellar content - novae, cataclysmic variables

Simbad objects: 9

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Number of rows : 9

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 M 31 G 00 42 44.330 +41 16 07.50 4.86 4.36 3.44     ~ 11049 1
2 NAME M31 RV No* 00 43 02.433 +41 12 56.17           M0 102 0
3 V* V838 Mon CV* 07 04 04.8222936785 -03 50 50.637499515   15.5   15.18 14.51 M10+B3V 375 0
4 M 99 H2G 12 18 49.625 +14 24 59.36 10.45 10.44 9.87     ~ 776 2
5 M 85 GiP 12 25 24.053 +18 11 27.89   10.2       ~ 604 0
6 NAME Vir I ClG 12 26 32.1 +12 43 24   10.00 8.49     ~ 5906 0
7 V* V1309 Sco CV* 17 57 32.9383021931 -30 43 09.967391199   16.9   14.8   ~ 181 0
8 V* V4332 Sgr CV* 18 50 36.6959119600 -21 23 28.927014456         14.37 K8/M0e 144 0
9 NAME Local Group GrG ~ ~           ~ 7067 0

    Equat.    Gal    SGal    Ecl

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2020.10.19-19:02:30

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