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The Progenitor of a Type Ia Supernova with a Short Delay Time?

Published online by Cambridge University Press:  17 January 2013

S. Mereghetti ,
N. La Palombara ,
A. Tiengo ,
P. Esposito ,
L. Stella  and
G.L. Israel
S. Mereghetti
Affiliation:
INAF, IASF-Milano, v. E.Bassini 15, I-20133 Milano, Italy email: sandro@iasf-milano.inaf.it
N. La Palombara
Affiliation:
INAF, IASF-Milano, v. E.Bassini 15, I-20133 Milano, Italy email: sandro@iasf-milano.inaf.it
A. Tiengo
Affiliation:
INAF, IASF-Milano, v. E.Bassini 15, I-20133 Milano, Italy email: sandro@iasf-milano.inaf.it IUSS, v.le Lungo Ticino Sforza 56, I-27100 Pavia, Italy
P. Esposito
Affiliation:
INAF - Osservatorio Astronomico di Cagliari, loc. Poggio dei Pini, strada 54, I-09012 Capoterra, Italy
L. Stella
Affiliation:
INAF - Osservatorio Astronomico di Roma, v. Frascati 33, I-00040 Monteporzio Catone, Italy
G.L. Israel
Affiliation:
INAF - Osservatorio Astronomico di Roma, v. Frascati 33, I-00040 Monteporzio Catone, Italy
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Abstract

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HD 49798/RX J0648.0-4418 is the only known X-ray binary composed of a hot subdwarf and a massive white dwarf (M=1.28 ± 0.05 M⊙). This system, with an orbital period of 1.55 days, is the outcome of a common envelope evolution, most likely of a pair of stars with initial masses of ~8–10M⊙. When the hot subdwarf, currently in a He-burning phase, will expand again and fill its Roche-lobe, the enhanced mass transfer can rapidly bring the already massive white dwarf above the Chandrasekhar limit. The possible final fate, either a Type Ia supernova explosion or an accretion induced collapse, is particularly interesting in view of the high rotational velocity of this star, which has the shortest spin period (13s) observed in a white dwarf.

Keywords

stars: subdwarfswhite dwarfsindividual (HD 49798) — X-rays: binariesindividual (RX J0648.0-4418)
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Issue S281: Binary Paths to Type Ia Supernovae Explosions , July 2011 , pp. 68 - 71
Copyright
Copyright © International Astronomical Union 2013

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