AB Doradus movement cluster

from Wikipedia, the free encyclopedia

The AB Doradus motion cluster contains about thirty young stars that have similarities in terms of their estimated age of 50 to 119 million years, their metallicity , and their common proper motion . The AB Doradus movement cluster is about 20  parsecs away and is therefore the closest movement cluster to the sun. With nine stars within ten parsecs, i.e. a little more than 30  light years , AB Doradus forms the core region of the movement cluster . Most of its smaller components are late K stars . Many of them could heat up even further or are still surrounded by dust. Six exoplanets have already been detected around the somewhat older neighbor of AB Doradus, HD 40307 , eight light years away . However, the system is not part of the movement group.

Due to its low age and its short distance, the AB-Doradus cluster of movements is ideally suited for the search for extrasolar planets as well as for researching the formation of planetary systems and their development around young stars, in addition to the regions around TW Hydrae and β Pictoris . With the latest techniques it should be possible to capture any components even pictorially.

Individual evidence

  1. ↑ VG Ortega, E. Jilinski, R. de la Reza, B. Bazzanella: On the common origin of the AB Doradus moving group and the Pleiades cluster . In: Monthly Notices of the Royal Astronomical Society . 377, No. 1, 2007, pp. 441-445. doi : 10.1111 / j.1365-2966.2007.11614.x .
  2. ↑ Ben Zuckerman, Inseok Song, MS Bessell: The AB Doradus Moving Group . In: The Astrophysical Journal . 613, No. 1, 2005, pp. L65-L68. doi : 10.1086 / 425036 .
  3. ↑ Mini-Invasion of Exoplanets - Article in Telepolis , June 17, 2008
  4. ↑ Planet HD 40307 g Astronomers marvel at Super-Earth. Spiegel Online, November 8, 2012, accessed November 8, 2012 .
  5. ↑ F. Hormuth, W. Brandner, S. Hippler; M. Janson, T. Henning: Direct imaging of the young spectroscopic binary HD 160934 . In: Astronomy and astrophysics . 463, No. 2, 2007, pp. 707-711. arxiv : astro-ph / 0612158 . doi : 10.1051 / 0004-6361: 20066765 .