Pith. sign in

REVIEW

The very short supersoft X-ray state of the classical nova M31N 2007-11a

Not yet reviewed by Pith; the record is open.

Re-run · record.json Download PDF Read on arXiv ↗

This paper has not been read by Pith yet. Machine review is queued; the pith claim, tier, and objections will appear here once it completes.

SPECIMEN: schema-true, not a live event

T0 review · schema-true

One-sentence machine reading of the paper's core claim.

pith:XXXXXXXX · record.json · timestamp

arxiv 0812.4420 v2 pith:E34G2PS2 submitted 2008-12-23 astro-ph

M. Henze , W. Pietsch , G. Sala , M. Della Valle , M. Hernanz , J. Greiner , V. Burwitz , M. J. Freyberg
show 4 more authors
F. Haberl D. H. Hartmann P. Milne G. G. Williams
This is my paper · ORCID
classification astro-ph
keywords x-raym31nopticaldaysnovashortveryclassical
verification ladder T0 review T1 audit T2 compute T3 formal
0 comments
read the original abstract

Short supersoft X-ray source (SSS) states (durations < 100 days) of classical novae (CNe) indicate massive white dwarfs that are candidate progenitors of supernovae type Ia. We carry out a dedicated optical and X-ray monitoring program of CNe in the bulge of M 31. We discovered M31N 2007-11a and determined its optical and X-ray light curve. We used the robotic Super-LOTIS telescope to obtain the optical data and XMM-Newton and Chandra observations to discover an X-ray counterpart to that nova. Nova M31N 2007-11a is a very fast CN, exhibiting a very short SSS state with an appearance time of 6-16 days after outburst and a turn-off time of 45-58 days after outburst. The optical and X-ray light curves of M31N 2007-11a suggest a binary containing a white dwarf with a mass greater than one solar mass.

Discussion (0). Continue with ORCID to comment.

Pith tools