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HD 61005
HD 61005 is a G8Vk class star〔( SIMBSD entry for HD61005 ).〕 in the constellation of Puppis with an associated accretion disk that has helped Astronomers understand the process of planetary formation. The particle size and asymmetrical shape of the accretion cloud, have forced a re-evaluation of traditional models of planet formation.〔Dean C. Hines, Glenn Schneider, David Hollenbach, Eric E. Mamajek, Lynne A. Hillenbrand, Stanimir Metchev, Michael R. Meyer, John M. Carpenter, Amaya Moro-Martín, Murray D. Silverstone, Jinyoung Serena Kim, Thomas Henning, Jeroen Bouwman, and Sebastian Wolf, (The Moth: An Unusual Circumstellar Structure Associated with HD 61005 ) The Astrophysical Journal 671 (2007) L165.〕〔S. Desidera et al. ''The debris disk host star HD 61005: a member of the Argus association?'' Astronomy & Astrophysics”. p529 (A54), May 2011〕
==Characteristics==
Although being a yellow dwarf like the sun, HD 61005 is much younger at just 135 million years old,〔V. Roccatagliata, Th. Henning, S. Wolf, J. Rodmann, S. Corder, J.M. Carpenter, M. Meyer and D. Dowell ( Long-wavelength observations of debris discs around sun-like stars ).〕 an extremely young age for stars. In this regard, the star retains a protoplanetary disk - the accumulation of the gas-dust matter, forming a planetary system. HD 61005 is located in the Local Bubble - a region with a low concentration of dust clouds.
HD 61005 is 115 light years from earth, has an apparent magnitude of 8.23 and a metalicity of 72.4% of the Sun. It is moving through the interstellar medium at a speed of 27.4 km/s relative to the Sun〔( HD 61005 (HIP 36948) ).〕 and is found in the night sky at right ascension 113.94248° and declination -32.20°.
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