Artist’s impression of the young massive star Cepheus A HW2. The narrow collimated jet originates from the embryonic star which lies at the centre of the image, hidden within a surrounding dust disc and larger disc of gas. The white lines indicate the 3-dimensional magnetic field structure along which material falls onto the slowly rotating discs.
Credit: Tobias Maercker.
A high-resolution version is also available.
An animation (4MB) shows the observations and the Cepheus A HW2 magnetic field. The spheres indicate velocity labelled methanol maser regions and the vectors indicate the 3-dimensional field direction determined for these masers. The thin and thick grey structures are the gas and dust disks respectively. The collimated radio outflows are indicated by the blue and red cones.
Magnetic control of massive stellar appetites
18 February 2010
A team of astronomers, led by Dr. Wouter Vlemmings at Bonn University, has used the MERLIN radio telescope network operated from Jodrell Bank to show that magnetic fields play an important role during the birth of massive stars. Magnetic fields are already known to strongly influence the formation of lower-mass stars like our Sun. This new study reveals that the way in which high-mass and low-mass stars form may be more similar than previously suspected. The scientists report their work in the journal Monthly Notices of the Royal Astronomical Society.
Massive stars, more than 8 times the mass of the Sun, are crucial to the formation of other stars, planets and even life. Though rare, they dominate the content and evolution of the interstellar material in the Galaxy and are responsible for the production of heavy elements such as iron. However, the question of how massive stars are formed has proved extremely difficult to answer. The role of magnetic fields in particular has been a topic of great debate. Many scientists thought that radiation and turbulence would be the more dominant factors, and hence their formation process would be significantly different from that of less massive stars such as our Sun.
"While magnetic fields have been observed in the molecular clouds from which the less heavy stars form, observations have been lacking close to massive stars," says Vlemmings. “If the formation of massive stars is similar to their lighter counterparts, we should be able to detect the strong magnetic fields needed to produce the jets and stabilize the disks that we see around lower mass stars.”
For the first time, Wouter Vlemmings and his collaborators have managed to observe the 3-dimensional magnetic field structure around the disk of the massive newly forming star (or protostar) Cepheus A HW2. At a distance of 2300 light years from the Sun, Cepheus A is one of the nearest regions where massive stars form and earlier observations of this region revealed the presence of a disk from which the gas falls on to HW2. In their new observations, the astronomers have found that the magnetic field is surprisingly regular and strong, implying that it is controlling how the matter is transferred through the disk to feed the growing embryonic star.
"Our new technique allows us for the first time to measure the 3D structure of the magnetic field around a massive protostar. We can see that its structure is surprisingly similar to how we think the field looks when much smaller stars form," adds co-author Huib Jan van Langevelde, director of the Joint Institute for Very Long BaseIine Interferometry in Europe (JIVE).
To determine the magnetic field structure, the researchers used the MERLIN telescope array to observe radio waves (with a wavelength of approximately 5 cm) that are amplified by methanol molecules. These methanol molecules, the simplest of the alcohol compounds, are found in regions surrounding the massive disk around HW2, which extend over a region 10 times the size of our Solar System. Such regions are called masers, because they amplify microwave radiation in the same way a laser amplifies light radiation. Even though a strong magnetic field produces only a very weak signature in the signal from the methanol molecules, this amplification is strong enough to make the new work possible.
These new observations will be a cornerstone of one of the first major scientific legacy projects to be carried out with the new e-MERLIN radio telescope network. e-MERLIN is a major upgrade to the MERLIN network that made it 10 times more sensitive. The legacy project, of which Dr. Vlemmings is one of the lead scientists, will use the unique capabilities of the upgraded network to reveal both the magnetic field and the immediate surroundings of many massive protostars of different ages.
A preprint of the paper is available from the astro-ph archive.
More information is available on the e-MERLIN legacy programme to study the formation of massive stars.
Dr. Wouter Vlemmings
Argelander-Institut für Astronomie, Universität Bonn, Germany
Tel: +49 228 733670 / 733658
Dr. Huib Jan van Langevelde
Joint Institute for VLBI in Europe, Dwingeloo, The Netherlands
Tel: +31 521 596524
Dr Robert Massey
Press and Policy Officer
Royal Astronomical Society
Tel: +44 (0)20 7734 3307
Mob: +44 (0)794 124 8035
MERLIN and e-MERLIN
MERLIN, operated from Jodrell Bank Observatory, is an array of up to seven radio telescopes distributed around the United Kingdom, with separations of up to 217km. MERLIN is operated by the University of Manchester as a National Facility of the UK Science and Technology Facilities Council. e-MERLIN is a major upgrade to MERLIN which incorporates new radio receivers at each telescope, new optical fibre links and associated hardware, and a new correlator to combine the signals.
Royal Astronomical Society
The Royal Astronomical Society press release is also available.