2016A&A...588A..88M


Query : 2016A&A...588A..88M

2016A&A...588A..88M - Astronomy and Astrophysics, volume 588A, 88-88 (2016/4-1)

The X-ray/radio and UV luminosity expected from symbiotic systems as the progenitor of SNe Ia.

MENG X. and HAN Z.

Abstract (from CDS):

Context. Symbiotic systems (i.e. a white dwarf + red giant star, WD + RG), which experience mass loss and form circumstellar material (CSM), have been suggested as being a possible progenitor system of type Ia supernovae (SNe Ia). After a supernova explosion, the supernova ejecta may interact with the CSM or the RG secondary. X-ray/radio emission (excess UV photons) is expected from the interaction between supernova ejecta and the CSM (RG secondary). However, no X-ray or radio emission that has originated from this type of system has been observationally detected, and only four SNe Ia have shown any possible signal of excess UV emission. These observational discrepancies need to be interpreted.
Aims. We seek to determine the luminosity of these emissions, using detailed binary evolution algorithms to obtain the parameters of binary systems at the moment of the supernova explosion.
Methods. We carried out a series of binary stellar evolution calculations, in which the effect of tidally enhanced wind on the evolution of WD + RG systems is incorporated. The WDs increase their mass to the Chandrasekhar mass limit, and then explode as SNe Ia. Based on the binary evolution results, we estimated the X-ray/radio (the excess UV) luminosity from the interactions between supernova ejecta and the CSM (the secondary) using a variety of published standard models.
Results. We found that the X-ray flux may be high enough to be detected for a nearby SN Ia from a symbiotic system, while the radio flux is more likely to de detected when the companion is an asymptotic giant branch (AGB) star, and for a first giant branch (FGB) companion, the radio flux is generally lower than the detection limit. For two well observed SNe Ia, 2011fe and 2014J, almost all symbiotic systems are excluded by X-ray observations, but WD + FGB systems may not be ruled out by radio observations. The excess UV luminosity that results from the collision of supernova ejecta with the RG secondary may be high enough to be detected if the secondary fills its Roche lobe at the moment of a supernova explosion.
Conclusions. The X-ray/radio emissions are more prevalent in SNe Ia from WD + AGB systems, although SNe Ia from such systems are rare. The UV luminosity from the collision of supernova ejecta to RG secondary is high enough, but only one in every few hundred SNe Ia manifests the signal from the collision.

Abstract Copyright: © ESO, 2016

Journal keyword(s): binaries: symbiotic - stars: evolution - supernovae: general - white dwarfs

Simbad objects: 15

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Number of rows : 15
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 SN 2002ic SN* 01 30 02.55 +21 53 06.9     18.5     SNIapec 224 1
2 SN 2009ig SN* 02 38 11.62 -01 18 45.3           SNIa 133 1
3 SN 2005gj SN* 03 01 11.96 -00 33 13.9   18.6       SNIapec 186 1
4 SN 2005ke SN* 03 35 04.35 -24 56 38.8     17.2     SNIap 132 1
5 SNR J050854-684447 SNR 05 08 58.7 -68 43 46           ~ 149 2
6 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 16002 1
7 SN 1993J SN* 09 55 24.77476 +69 01 13.7026   10.8 12.0     SNIIb 1325 1
8 SN 2014J SN* 09 55 42.12 +69 40 25.9           SNIa 358 1
9 SN 2006X SN* 12 22 53.93 +15 48 32.0     15.3     SNIa 300 1
10 SN 2012cg SN* 12 27 12.83 +09 25 13.2           SNIa 156 1
11 iPTF 14atg SN* 12 52 44.8 +26 28 13           SNIa 61 0
12 SN 2011fe SN* 14 03 05.711 +54 16 25.22   10.12 10.06     SNIa 583 1
13 SN 2011de SN* 15 43 53.25 +67 45 42.5           SNIa(N) 12 1
14 V* T CrB Sy* 15 59 30.1622265912 +25 55 12.613382940   11.516 10.247 9.70   M3IIIe_sh 674 0
15 V* RS Oph Sy* 17 50 13.1591484960 -06 42 28.480729788   11.884 10.776 11.228   K5.5/M0IIIe 1006 0

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2022.05.27-20:20:41

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