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A classical nova, V2487 Oph 1998, seen in x-rays before and after its explosion.
Margarita Hernanz1, Glòria Sala
1Institut d'Estudis Espacials de Catalunya and Instituto de Ciencias del Espacio, Consejo Superior de Investigaciones Científicas, Gran Capità 2-4, E-08034 Barcelona, Spain. hernanz@ieec.fcr.es
Science (New York, N.Y.)
|October 12, 2002
Summary
Recent observations show that accretion onto a white dwarf star, the cause of classical nova explosions, resumed just 2.7 years after the V2487 Oph 1998 event. This suggests the nova site was previously observed in X-rays.
Area of Science:
- * Astronomy and astrophysics
- * Stellar evolution and explosive phenomena
Background:
- * Classical novae result from thermonuclear runaway on accreting white dwarfs.
- * Understanding the post-outburst evolution of novae is crucial for stellar physics.
Purpose of the Study:
- * To investigate the re-establishment of accretion in the classical nova V2487 Oph 1998.
- * To determine if the nova progenitor system was previously observed in X-rays.
Main Methods:
- * Analysis of X-ray Multi-Mirror satellite (XMM-Newton) observations of V2487 Oph 1998.
- * Positional correlation with archival data from the Röntgen Satellite (ROSAT).
Main Results:
- * Evidence of accretion re-established on a white dwarf 2.7 years post-outburst.
- * Identification of a potential pre-outburst X-ray source at the nova's location.
Conclusions:
- * Accretion can resume relatively quickly after a classical nova explosion.
- * Pre-outburst X-ray observations may reveal sites of future novae.