TY - JOUR
T1 - V445 puppis
T2 - Helium nova on a massive white dwarf
AU - Kato, Mariko
AU - Hachisu, Izumi
N1 - Funding Information:
We are grateful to VSNET members who contributed to the V445 Pup light curve. This work was supported in part by the Grants-in-Aid from the 21st Century Center of Excellence program (Research Center for Integrated Science) of the Minister of Education, Culture, Sports, Science, and Technology, Japan.
PY - 2003/12/1
Y1 - 2003/12/1
N2 - The 2000 outburst of V445 Puppis shows unique properties, such as the absence of hydrogen, the enrichment of helium and carbon, and the slow development of the light curve with a small amplitude that does not resemble any classical novae. This object has been suggested to be the first example of a helium nova. We calculate theoretical light curves of helium novae and reproduce the observational light curve of V445 Pup. Modeling indicates a very massive white dwarf (WD), more massive than 1.3 M⊙. The companion star is possibly either a helium star or a helium-rich main-sequence star. We estimate the ignition mass as several times 10-5 M ⊙, the corresponding helium accretion rate as several times 10-7 M⊙ yr-1, and the recurrence period as several tens of years. These values suggest that the WD is growing in mass and ends up either a Type la supernova or an accretion-induced collapse to a neutron star.
AB - The 2000 outburst of V445 Puppis shows unique properties, such as the absence of hydrogen, the enrichment of helium and carbon, and the slow development of the light curve with a small amplitude that does not resemble any classical novae. This object has been suggested to be the first example of a helium nova. We calculate theoretical light curves of helium novae and reproduce the observational light curve of V445 Pup. Modeling indicates a very massive white dwarf (WD), more massive than 1.3 M⊙. The companion star is possibly either a helium star or a helium-rich main-sequence star. We estimate the ignition mass as several times 10-5 M ⊙, the corresponding helium accretion rate as several times 10-7 M⊙ yr-1, and the recurrence period as several tens of years. These values suggest that the WD is growing in mass and ends up either a Type la supernova or an accretion-induced collapse to a neutron star.
KW - Binaries: close
KW - Novae, cataclysmic variables
KW - Stars: individual (V445 Puppis)
KW - White dwarfs
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U2 - 10.1086/380597
DO - 10.1086/380597
M3 - Article
AN - SCOPUS:0346969694
SN - 0004-637X
VL - 598
SP - L107-L110
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 2 II
ER -