UvA Astronomy students offer new insight into gaseous and dust discs around stars
27 October 2010
Research by two Master's students from the University of Amsterdam's (UvA) Anton Pannekoek Astronomical Institute (IAP), offers new insight into the structure of the gaseous and dust disc around a so-called ‘Herbig Be' star, leading to an article in the scientific journal 'Astrophysical Journal Letters'.
Research by two Master's students from the University of Amsterdam's (UvA) Anton Pannekoek Astronomical Institute (IAP), offers new insight into the structure of the gaseous and dust disc around a so-called ‘Herbig Be' star. The measurements taken by the students have led to an article in the scientific journal Astrophysical Journal Letters, which was published this week.
Students Rik van Lieshout and Tullio Bagnoli performed measurements at the observatory on La Palma (Canary Islands). They did this for the Observation Project, part of the UvA's Astronomy and Astrophysics Master's study programme, after first submitting an observation proposal. They studied the Herbig Be star MWC 147, a very young, newly formed star in the transitional stage between massive and less massive stars. The mass of this star is approximately six times the mass of the Sun. The question the students wanted to answer is whether stars much heavier than the Sun are able to form planets.
Herbig Be stars are surrounded by a disk with gaseous and solid particles. The measurements, which Van Lieshout and Bagnoli made with the Belgian Mercator telescope, offer new insight into the structure of the gaseous and dust disc near the star, at a spatial scale much smaller than the orbit of Mercury around the Sun. Planets could possibly be formed in the aforementioned disc. Observations on this scale are usually done with the world's largest telescopes. Thanks to a new instrument developed by staff from the K.U. Leuven, Van Lieshout and Bagnoli could make these measurements with a smaller telescope. Thus, they could describe the physical properties of the gaseous and dust disc, including the geometry and surface brightness. There is an inner and outer disk. The inner disc is flat and appears to pass close the star surface, while the outer disk is much thicker and has a conical shape (the shape of a horn). The inner disc consists entirely of gaseous, due to the high temperature as a result of proximity to MWC 147 (too hot for dust particles). The transition between these two parts of the disk is consistent with earlier findings.
The question is whether stars much heavier than the Sun are able to form planets. The formation of rocky planets through the accumulation of dust grains does not seem possible in the inner flat portion of the disk around MWC 147 because no dust grains can exist there. The dimensions of this flat portion of the disc roughly correspond to the distance between the Sun and Mars in our solar system. A better understanding of planet formation may lead to greater understanding of the formation of our solar system. This requires mapping out the structure of the gaseous and dust disc (the protoplanetary disc, where planets may come into being) from other stars.
The students were accompanied by Prof. Rens Waters (Professor of Astronomy at the University of Amsterdam and Scientific Director of SRON Netherlands Institute for Space Research) and Gerrit van der Plas and Daan Meerburg (both PhD students at the UvA's IAP). In addition, researchers from K.U. Leuven's Institute of Astronomy (Belgium) also contributed to the piece in Astrophysical Journal Letters.
T. Bagnoli, R. van Lieshout, L.B.F.M. Waters, G. van der Plas, B. Acke, H. van Winckel, G. Raskin and P.D. Meerburg: 'An inner gaseous disk around the Herbig Be star MWC 147', in: Astrophysical Journal Letters, 22 October, 2010.