Andrew Yee[_1_]
June 10th 07, 03:45 PM
ESA News
http://www.esa.int
31 May 2007
XMM-Newton reveals X-rays from gas streams around young stars
XMM-Newton has surveyed nearly two hundred stars under formation to reveal,
contrary to expectations, how streams of matter fall onto the young stars'
magnetic atmospheres and radiate X-rays.
The results defy astronomers' expectations, as the streams of falling matter
interact with the hot corona, cooling it, while the ejected streams of gas
heat up in shocks as they are ejected from the star.
The new XMM-Newton results paint a dramatic picture of the role magnetic
fields play in star formation. "Star formation is a battle between gravity
and everything else," says Manuel Guedel, Paul Scherrer Institut, Villigen,
Switzerland, who leads a large project addressing magnetic activity in young
stars within the constellation of Taurus.
Star formation results in a complicated system in which the young star is
surrounded by a disc of gas and dust. This matter then follows one of three
different routes. It finds its way onto the star through magnetic funnels,
or stays in the disc to form planets, or is thrown clear of the system in a
wind or jet created by the overall magnetic field.
With the help of ESA's X-ray observatory XMM-Newton, Guedel and his 25
international colleagues are now ready to report new details from the front
line.
They used XMM-Newton to target stars in the nearby Taurus Molecular Cloud.
This vast cloud in space is one of the star-forming regions nearest to Earth
and contains over 400 young stars.
Most of these stars are still accumulating matter, a process known as
accretion. As falling matter strikes the surface of the star, it typically
doubles the temperature of the surface from 5000 Kelvin to 10 000 Kelvin.
This produces an excessive amount of ultraviolet radiation emitted by the
star and detected by XMM-Newton's Optical Monitor. Astronomers had thought
that the same shock waves that caused the emission of the ultraviolet excess
should also produce an excess of X-rays.
Confusingly enough, previous observations seemed to show that young stars
that still accrete matter give off less X-ray emission. To investigate this
mystery, amongst several others, ESA approved a large programme of
observations with XMM-Newton. The space-borne observatory investigated the
densest regions of the Taurus Molecular Cloud for a total of more than 7
days.
The new results from XMM-Newton propose a solution to the mystery. In
addition, they bring forward unanticipated discoveries. "We have not seen
the expected X-rays that the shocks should produce on the surface of some
stars," says Guedel.
Instead, XMM-Newton's spectrometers revealed a new and subtle feature
suggesting that the falling material cooled the hot X-ray emitting
atmosphere of the young stars, suppressing the emission of X-rays.
In certain cases, namely in the more heavily accreting stars, the
suppression of the X-rays was such that the team realised that an additional
process was at work in these objects. In addition to cooling the outer
stellar atmosphere, the gas streams falling onto the star were so dense that
they absorbed most of the X-rays that the star's atmosphere had emitted.
Although such dense streams of gas should also contain dust that would
obscure the star at visible wavelengths, the star is seen shining brightly.
So what happens to this dust? The team can propose an answer to this as
well. "The dust is heated so much by the radiation from the star, that it is
vaporised before it can fall on the star," says Guedel.
The strong X-ray suppression allowed the team to discover yet another X-ray
source associated with the same stars coming from relatively cool gas that
does not suffer from absorption. "This emission must come from outside the
accretion streams," says Guedel. The team interprets the X-rays as evidence
that some gas streams ejected by the star form shock waves that heat up very
strongly.
The work gives astronomers powerful new insight into the tremendous forces
at work in star formation.
Note to editors:
A collection of 15 papers reporting the above results and many others is
published in Astronomy and Astrophysics on 31 May 2007.
Taurus Molecular Cloud project page:
http://www.issibern.ch/teams/Taurus
The XMM-Newton Extended Survey of the Taurus Molecular Cloud (XEST project
has been conducted by an international team under the leadership of the Paul
Scherrer Institute in Switzerland.
Co-investigator institutes were the Laboratoire d'Astrophysique de Grenoble,
the INAF/ Osservatorio Astronomico di Palermo, the University of Geneva,
Columbia University, Penn State University at University Park, the
California Institute of Technology, the INAF/ Osservatorio Astrofisico di
Arcetri in Florence, the Max-Planck-Institut f Radioastronomie, the
University of Porto, and the University of Colorado at Boulder. The project
was partly supported by the International Space Science Institute in Bern,
Switzerland.
For more information:
Manuel Guedel, Paul Scherrer Institut, Villigen, Switzerland
Email: guedel @ astro.phys.ethz.ch
Norbert Schartel, XMM-Newton Project Scientist
Norbert.schartel @ sciops.esa.int
[NOTE: Images supporting this release are available at
http://www.esa.int/esaCP/SEMX379RR1F_index_1.html ]
http://www.esa.int
31 May 2007
XMM-Newton reveals X-rays from gas streams around young stars
XMM-Newton has surveyed nearly two hundred stars under formation to reveal,
contrary to expectations, how streams of matter fall onto the young stars'
magnetic atmospheres and radiate X-rays.
The results defy astronomers' expectations, as the streams of falling matter
interact with the hot corona, cooling it, while the ejected streams of gas
heat up in shocks as they are ejected from the star.
The new XMM-Newton results paint a dramatic picture of the role magnetic
fields play in star formation. "Star formation is a battle between gravity
and everything else," says Manuel Guedel, Paul Scherrer Institut, Villigen,
Switzerland, who leads a large project addressing magnetic activity in young
stars within the constellation of Taurus.
Star formation results in a complicated system in which the young star is
surrounded by a disc of gas and dust. This matter then follows one of three
different routes. It finds its way onto the star through magnetic funnels,
or stays in the disc to form planets, or is thrown clear of the system in a
wind or jet created by the overall magnetic field.
With the help of ESA's X-ray observatory XMM-Newton, Guedel and his 25
international colleagues are now ready to report new details from the front
line.
They used XMM-Newton to target stars in the nearby Taurus Molecular Cloud.
This vast cloud in space is one of the star-forming regions nearest to Earth
and contains over 400 young stars.
Most of these stars are still accumulating matter, a process known as
accretion. As falling matter strikes the surface of the star, it typically
doubles the temperature of the surface from 5000 Kelvin to 10 000 Kelvin.
This produces an excessive amount of ultraviolet radiation emitted by the
star and detected by XMM-Newton's Optical Monitor. Astronomers had thought
that the same shock waves that caused the emission of the ultraviolet excess
should also produce an excess of X-rays.
Confusingly enough, previous observations seemed to show that young stars
that still accrete matter give off less X-ray emission. To investigate this
mystery, amongst several others, ESA approved a large programme of
observations with XMM-Newton. The space-borne observatory investigated the
densest regions of the Taurus Molecular Cloud for a total of more than 7
days.
The new results from XMM-Newton propose a solution to the mystery. In
addition, they bring forward unanticipated discoveries. "We have not seen
the expected X-rays that the shocks should produce on the surface of some
stars," says Guedel.
Instead, XMM-Newton's spectrometers revealed a new and subtle feature
suggesting that the falling material cooled the hot X-ray emitting
atmosphere of the young stars, suppressing the emission of X-rays.
In certain cases, namely in the more heavily accreting stars, the
suppression of the X-rays was such that the team realised that an additional
process was at work in these objects. In addition to cooling the outer
stellar atmosphere, the gas streams falling onto the star were so dense that
they absorbed most of the X-rays that the star's atmosphere had emitted.
Although such dense streams of gas should also contain dust that would
obscure the star at visible wavelengths, the star is seen shining brightly.
So what happens to this dust? The team can propose an answer to this as
well. "The dust is heated so much by the radiation from the star, that it is
vaporised before it can fall on the star," says Guedel.
The strong X-ray suppression allowed the team to discover yet another X-ray
source associated with the same stars coming from relatively cool gas that
does not suffer from absorption. "This emission must come from outside the
accretion streams," says Guedel. The team interprets the X-rays as evidence
that some gas streams ejected by the star form shock waves that heat up very
strongly.
The work gives astronomers powerful new insight into the tremendous forces
at work in star formation.
Note to editors:
A collection of 15 papers reporting the above results and many others is
published in Astronomy and Astrophysics on 31 May 2007.
Taurus Molecular Cloud project page:
http://www.issibern.ch/teams/Taurus
The XMM-Newton Extended Survey of the Taurus Molecular Cloud (XEST project
has been conducted by an international team under the leadership of the Paul
Scherrer Institute in Switzerland.
Co-investigator institutes were the Laboratoire d'Astrophysique de Grenoble,
the INAF/ Osservatorio Astronomico di Palermo, the University of Geneva,
Columbia University, Penn State University at University Park, the
California Institute of Technology, the INAF/ Osservatorio Astrofisico di
Arcetri in Florence, the Max-Planck-Institut f Radioastronomie, the
University of Porto, and the University of Colorado at Boulder. The project
was partly supported by the International Space Science Institute in Bern,
Switzerland.
For more information:
Manuel Guedel, Paul Scherrer Institut, Villigen, Switzerland
Email: guedel @ astro.phys.ethz.ch
Norbert Schartel, XMM-Newton Project Scientist
Norbert.schartel @ sciops.esa.int
[NOTE: Images supporting this release are available at
http://www.esa.int/esaCP/SEMX379RR1F_index_1.html ]