X-rays provide a new way to investigate exploding stars
Wed May 9, 2007 at 20:39 UTC
ESA's X-ray observatory XMM-Newton has revealed a new class of exploding stars – where the X-ray emission 'lives fast and dies young'. The identification of this particular class of explosions gives astronomers a valuable new constraint to help them model and understand stellar explosions.
Exploding stars called novae remain a puzzle to astronomers. "Modelling these outbursts is very difficult," says Wolfgang Pietsch of the Max Planck Institut für Extraterrestrische Physik. Now, ESA's XMM-Newton and NASA's Chandra space-borne X-ray observatories have provided valuable information about when individual novae emit X-rays.
Between July 2004 and February 2005, the X-ray observatories watched the heart of the nearby galaxy, Andromeda, also known to astronomers as M31. During that time, Pietsch and his colleagues monitored novae, looking for the X-rays.
They detected that eleven out of the 34 novae that had exploded in the galaxy during the previous year were shining X-rays into space. "X-rays are an important window onto novae. They show the atmosphere of the white dwarf," says Pietsch.
White dwarfs are hot stellar corpses left behind after the rest of the star has been ejected into space. A typical white dwarf contains about the mass of the Sun, in a spherical volume little bigger than the Earth. Given its density, it has a strong pull of gravity. If in orbit around a normal star, it may rip gas from the star.
This material builds up on the surface of the white dwarf until it reaches sufficient density for a nuclear detonation. The resultant explosion creates a nova visible in the optical region for a few to a hundred days. However, these particular events are not strong enough to destroy the underlying white dwarf.
The X-ray emission becomes visible some time after the detonation, when the matter ejected by the nova thins out. This allows astronomers to peer down to the atmosphere of the white dwarf, which is burning by nuclear fusion.
At the end of the process, the X-ray emission stops when the fuel is exhausted. The duration of this X-ray emission traces the amount of material left on the white dwarf after the nova has ended.
Image Credit: W. Pietsch (MPE Garching, Germany), ESA/XMM Newton
This image is a mosaic of XMM-Newton's European Photon Imaging Camera's (EPIC) observations of the central region of M31 as seen from 2000 to 2004.
The color coding is such that red displays X-ray photons received in the energy band 0.2-0.5 keV, green in the 0.5-1 keV band and blue in the 1-2 keV band. The positions of ten counterparts of optical novae detected in these images are indicated with circles and nova names. Nova names are given omitting the M31N prefix.
It was detected that eleven out of the 34 novae that had exploded in the galaxy during the previous year were shining X-rays into space. An additional seven novae remained detectable in X-rays up to 10 years after outburst.
The conclusion of the scientists is that the number of X-ray-detected optical novae is higher than previously expected, an important indication of the physical properties of these systems. The short-lived optical novae form a new 'live fast and die young' class of X-ray sources that would have been overlooked in the past by surveys carried out only every six months.
To investigate further, the team have been awarded more XMM-Newton and Chandra observing time. They now plan to monitor M31's novae every ten days for several months, starting in November 2007.
Image Credit: W. Pietsch (MPE Garching, Germany), P. Massey (Lowell Observatory, USA), NASA/Chandra
This is an optical H-alpha image overplotted with contours from Chandra observations.
The optical image of the central area of M31 was taken with the 4-metre Kitt Peak National Observatory telescope during the Local Group Survey. The overlying contours are taken from merged observations of the Chandra High Resolution Camera in the imaging mode (HRC-I) carried out from December 2004 to February 2005.
The positions of 17 counterparts of optical novae detected in these images are indicated with circles and nova names. Nova names are given omitting the M31N prefix. The cross between the novae M31N 1995-09b and M31N 2004-11f indicates the centre of M 31 center, the point aimed at for observation.
A well determined start time of the optical nova outburst and the X-ray turn-on and turn-off times are therefore important benchmarks, or constraints, for replication in computer models of novae.
Whilst monitoring the M31 novae frequently over several months for the appearance and subsequent disappearance of the X-rays, Pietsch made an important discovery. Some novae started to emit X-rays and then turned them off again within just a few months.
"These novae are a new class. They would have been overlooked before," says Pietsch. That's because previous surveys looked only every six months or so. Within that time, the fast X-ray novae could have blinked both on and off.
In addition to discovering the short-lived ones, the new survey also confirms that other novae generate X-rays over a much longer time. XMM-Newton detected seven novae that were still shining X-rays into space, up to a decade after the original eruption.
The differing lengths of times are thought to reflect the masses of the white dwarfs at the heart of the nova explosion. The fastest evolving novae are thought to be those coming from the most massive white dwarfs.
To investigate further, the team, lead by Dr. Pietsch, have been awarded more XMM-Newton and Chandra observing time. They now plan to monitor M31's novae every ten days for several months, starting in November 2007, to glean more information about these puzzling stellar explosions.
European Space Agency News Release
