A theoretical systematic study of nova light curves

2014 Fiscal Year Final Research Report

• Project/Area Number: 22540254
• Research Category: Grant-in-Aid for Scientific Research (C)
• Allocation Type: Single-year Grants
• Section: 一般
• Research Field: Astronomy
• Research Institution: Keio University
• Principal Investigator: KATO Mariko 慶應義塾大学, 理工学部, 教授 (50185873)
• Project Period (FY): 2010-04-01 – 2015-03-31
• Keywords: 新星 / 白色矮星 / 連星系

Outline of Final Research Achievements

We found that, for less massive white dwarfs (WDs), the opticaly thick wind does not occur throughout the outburst or if it does it begins after a delay time for a transition. We also found the general evolution course in the color-color diagram (nova-giant sequence) that is common for various types of nova. This property is useful to estimate the interstellar extinction and distance. In the light curve analysis of slow novae, the contribution of photospheric emission cannot be neglected, whereas in the fast novae the free-free emission dominates. Novae in globular clusters may contain only massive WDs because of weak acceleration of the winds. We also calculated binary evolution including super-Chandrasekhar WD mass.

Free Research Field

天体物理学