一颗经典新星，1998年蛇夫座V2487，在爆发前后均被观测到X射线。

A classical nova, V2487 Oph 1998, seen in x-rays before and after its explosion.

作者信息

Hernanz Margarita, Sala Glòria

机构信息

Institut d'Estudis Espacials de Catalunya and Instituto de Ciencias del Espacio, Consejo Superior de Investigaciones Científicas, Gran Capità 2-4, E-08034 Barcelona, Spain.

出版信息

Science. 2002 Oct 11;298(5592):393-5. doi: 10.1126/science.298.5592.393.

DOI:10.1126/science.298.5592.393

PMID:12376696

Abstract

Classical nova explosions are very energetic and frequent phenomena caused by explosive hydrogen burning on top of an accreting white dwarf. Observations of the recent nova V2487 Oph 1998 by the X-ray Multi-Mirror satellite (XMM-Newton) provide evidence that accretion (probably on a magnetic white dwarf) was reestablished as early as 2.7 years after the explosion. In addition, positional correlation with a source previously discovered by the Röntgen Satellite (ROSAT) in 1990 suggests that the site of a nova explosion had been seen in x-rays before the outburst.

摘要

经典新星爆发是由吸积白矮星表面的氢爆发燃烧引起的能量巨大且频繁的现象。X射线多镜面卫星（XMM-牛顿卫星）对近期的1998年蛇夫座V2487新星的观测提供了证据，表明早在爆发后2.7年吸积（可能是在一颗磁白矮星上）就已重新建立。此外，与伦琴卫星（ROSAT）在1990年先前发现的一个源的位置相关性表明，在爆发之前新星爆发的位置就已在X射线中被观测到。