Nova Herculis 1991
Image courtesy of the Max Planck Institute.
Nova Herculis 1991, shown in this PSPC image, is a fast, high inclination, long period nova which contains a massive white dwarf and is part of an eclipsing binary system. Novae occur as part of the evolution of a close binary system in which the stars have different masses, i.e. a main sequence star and a white dwarf. Mass is accreted onto the white dwarf which eventually ignites runaway thermonuclear reactions which blow off the outer layers of the star. This particular nova (also known as V838 Her) was discovered by independent Japanese and British amateur astronomers March 24/25 of 1991. ROSAT observations were made five days after discovery and again one year later.
|
Search for an Image: (Enter the name of an object.) | Additions or Comments: Have we left anything out? Is there something you would like to have added to this page (a link to your own group's research page, for example...)? |
OBJECTS | By Mission | Stars | Cataclysmic Variables | X-ray Binaries | Pulsars | Supernova Remnants | Galaxies | Active Galactic Nuclei | Clusters of Galaxies | X-ray Background | Planets, Comets, etc. | Gamma Ray Bursts
HEASARC Home | Observatories | Data Archive | Software | Utilities | Helpdesk/FAQ | Education & Outreach
Imagine! | StarChild | Ask a High-Energy Astronomer | WebStars | APOD: Astronomy Picture of the Day | HEAPOW: High-Energy Astrophysics Picture of the Week | Images | Video Archive
|
Space Science Data System
Part of the NASA OSS
Questions/Comments/Feedback
|
A service of the
Laboratory for High Energy Astrophysics (LHEA)
at
NASA/
GSFC and the High Energy Astrophysics Division of the Smithsonian Astrophysical Observatory (SAO)
HEASARC Director:
Dr. Nicholas E. White, |