2017MNRAS.471.3200M


C.D.S. - SIMBAD4 rel 1.7 - 2020.10.31CET12:34:18

2017MNRAS.471.3200M - Mon. Not. R. Astron. Soc., 471, 3200-3211 (2017/November-1)

Shock-powered light curves of luminous red novae as signatures of pre-dynamical mass-loss in stellar mergers.

METZGER B.D. and PEJCHA O.

Abstract (from CDS):

Luminous red novae (LRN) are a class of optical transients believed to originate from the mergers of binary stars, or 'common envelope' events. Their light curves often show secondary maxima, which cannot be explained in the previous models of thermal energy diffusion or hydrogen recombination without invoking multiple independent shell ejections. We propose that double-peaked light curves are a natural consequence of a collision between dynamically ejected fast shell and pre-existing equatorially focused material, which was shed from the binary over many orbits preceding the dynamical event. The fast shell expands freely in the polar directions, powering the initial optical peak through cooling envelope emission. Radiative shocks from the collision in the equatorial plane power the secondary light-curve peak on the radiative diffusion time-scale of the deeper layers, similar to luminous Type IIn supernovae and some classical novae. Using a detailed 1D analytic model, informed by complementary 3D hydrodynamical simulations, we show that shock-powered emission can explain the observed range of peak time-scales and luminosities of the secondary peaks in LRN for realistic variations in the binary parameters and fraction of the binary mass ejected. The dense shell created by the radiative shocks in the equatorial plane provides an ideal location for dust nucleation consistent with the inferred aspherical geometry of dust in LRN. For giant stars, the ejecta forms dust when the shock-powered luminosity is still high, which could explain the infrared transients recently discovered by Spitzer. Our results suggest that pre-dynamical mass-loss is common if not ubiquitous in stellar mergers, providing insight into the instabilities responsible for driving the binary merger.

Abstract Copyright: © 2017 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society

Journal keyword(s): binaries: close - stars: evolution - stars: evolution

Simbad objects: 11

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Number of rows : 11

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 NAME M31 RV No* 00 43 02.433 +41 12 56.17           M0 102 0
2 SN 1987A SN* 05 35 28.020 -69 16 11.07           SNIIpec 4525 2
3 V* V838 Mon CV* 07 04 04.8222936785 -03 50 50.637499515   15.5   15.18 14.51 M10+B3V 376 0
4 * eta Car Em* 10 45 03.5455050 -59 41 03.951060 6.37 7.034 6.21 4.90 4.41 OBepec 2222 0
5 NAME NGC 4490-OT2011 ev 12 30 41.85 +41 37 49.8           ~ 27 0
6 SPIRITS14ajc ev 13 36 52.95 -29 52 16.1           ~ 4 0
7 NAME M101 OT2015-1 SN? 14 02 16.78 +54 26 20.5   19.19 17.57 16.92 16.26 ~ 33 0
8 PSN J14595947+0154262 SN? 14 59 59.47 +01 54 26.6           ~ 25 1
9 V* V1309 Sco CV* 17 57 32.9383021931 -30 43 09.967391199   16.9   14.8   ~ 183 0
10 EWS 2002-BLG-360 CV* 17 57 38.98752 -29 46 05.1636           ~ 29 0
11 V* V4332 Sgr CV* 18 50 36.6959119600 -21 23 28.927014456         14.37 K8/M0e 146 0

    Equat.    Gal    SGal    Ecl

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2020.10.31-12:34:18

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