A PREDICTION FORMULA OF SUPERSOFT X-RAY PHASE OF CLASSICAL NOVAE

Journal Article · Mon Feb 01 04:00:00 EST 2010 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/709/2/680· OSTI ID:21392318

Hachisu, Izumi ^[1]; Kato, Mariko ^[2]

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1. Department of Earth Science and Astronomy, College of Arts and Sciences, University of Tokyo, Komaba, Meguro-ku, Tokyo 153-8902 (Japan)
2. Department of Astronomy, Keio University, Hiyoshi, Kouhoku-ku, Yokohama 223-8521 (Japan)

On the basis of the recently developed universal decline law of classical novae, we propose prediction formulae for supersoft X-ray on and off times, i.e., t{sub X-on} = (10 +- 1.8)t{sub 3} days and t{sub X-off} = (5.3 +- 1.4)(t{sub 3}){sup 1.5} days for 8 approx< t{sub 3} approx< 80 days. Here t{sub 3} is the newly proposed 'intrinsic' decay time during which the brightness drops by 3 mag from optical maximum along our universal decline law fitted with observation. We have determined the absolute magnitude of our free-free emission model light curves and derived maximum magnitude versus rate of decline (MMRD) relations. Our theoretical MMRD relations are governed by two parameters, one is the white dwarf (WD) mass and the other is the initial envelope mass at a nova outburst; this second parameter explains the scatter of MMRD points of individual novae. Our theoretical MMRD relations are also in good agreement with the well-known empirical formulae. We also show another empirical relation of M{sub V} (15) approx -5.7 +- 0.3 based on the absolute magnitude of our model light curves, i.e., the absolute magnitude at 15 days after optical maximum is almost common among various novae. We analyzed 10 nova light curves, in which a supersoft X-ray phase was detected, and estimated their WD masses. The models best simultaneously reproducing the optical and supersoft X-ray observations are ONeMg WDs with 1.28 +- 0.04 M{sub sun} (V598 Pup), 1.23 +- 0.05 M{sub sun} (V382 Vel), 1.15 +- 0.06 M{sub sun} (V4743 Sgr), 1.13 +- 0.06 M{sub sun} (V1281 Sco), 1.2 +- 0.05 M{sub sun} (V597 Pup), 1.06 +- 0.07 M{sub sun} (V1494 Aql), 1.04 +- 0.07 M{sub sun} (V2467 Cyg), 1.07 +- 0.07 M{sub sun} (V5116 Sgr), 1.05 +- 0.05 M{sub sun} (V574 Pup), and a CO WD with 0.93 +- 0.08 M{sub sun} (V458 Vul). The newly proposed relationships are consistent with the emergence or decay epoch of the supersoft X-ray phase of these 10 novae. Finally, we discuss the mechanism of shock-origin hard X-ray component in relation to the emergence of companion star from the WD envelope.

• OSTI ID: 21392318
• Journal Information: Astrophysical Journal, Journal Name: Astrophysical Journal Journal Issue: 2 Vol. 709; ISSN ASJOAB; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTRONOMY AND ASTROPHYSICS
BINARY STARS
BRIGHTNESS
DWARF STARS
ELECTROMAGNETIC RADIATION
EMISSION
ERUPTIVE VARIABLE STARS
HARD X RADIATION
IONIZING RADIATIONS
MASS
NOVAE
OPTICAL PROPERTIES
PHYSICAL PROPERTIES
RADIATIONS
STARS
VARIABLE STARS
WHITE DWARF STARS
X RADIATION