Exozodiacal dust

From Wikipedia, the free encyclopedia
Jump to: navigation, search
This artist’s view from an imagined planet around a nearby star shows the brilliant glow of exozodiacal light extending up into the sky and swamping the Milky Way.

Exozodiacal dust is the exoplanetary analog of zodiacal dust, the 1–100 micrometre-sized grains of amorphous carbon and silicate dust that fill the plane of the solar system, especially interior to the asteroid belt. As for the zodiacal dust, these grains are probably produced by outgassing comets, as well as by collisions among bigger parent bodies like asteroids. Exozodiacal dust clouds are often components of debris disks that are detected around main-sequence stars through their excess infrared emission. By convention, exozodiacal dust refers to the innermost and hottest part of these debris disks, within a few astronomical units from the star. The shapes of exozodiacal dust clouds can show the dynamical influence of extrasolar planets, and potentially indicate the presence of these planets.[1] Because it is located near a star's habitable zone, exozodiacal dust can be an important noise source for attempts to image terrestrial planets.

Examples of stars with exozodiacal dust[edit]


  1. ^ Stark, C..; Kuchner, M. (2008). "The Detectability of Exo-Earths and Super-Earths Via Resonant Signatures in Exozodiacal Clouds". The Astrophysical Journal 686 (1): 637–648. arXiv:0810.2702. Bibcode:2008ApJ...686..637S. doi:10.1086/591442. 
  2. ^ Lebreton, J.; van Lieshout, R.; Augereau, J.-C.; Absil, O.; Mennesson, B.; Kama, M.; Dominik, C.; Bonsor, A.; Vandeportal, J.; Beust, H.; Defrère, D.; Ertel, S.; Faramaz, V.; Hinz, P.; Kral, Q.; Lagrange, A.-M.; Liu, W.; Thébault, P. (2013). "An interferometric study of the Fomalhaut inner debris disk. III. Detailed models of the exozodiacal disk and its origin". Astronomy and Astrophysics 555. arXiv:1306.0956. Bibcode:2013A&A...555A.146L. doi:10.1051/0004-6361/201321415. 
  3. ^ a b Absil, O.; Le Bouquin, J.-B.; Berger, J.-P.; Lagrange, A.-M.; Chauvin, G.; Lazareff, B.; Zins, G.; Haguenauer, P.; Jocou, L.; Kern, P.; Millan-Gabet, R.; Rochat, S.; Traub, W. (2011). "Searching for faint companions with VLTI/PIONIER. I. Method and first results". Astronomy and Astrophysics 535. arXiv:1110.1178. Bibcode:2011A&A...535A..68A. doi:10.1051/0004-6361/201117719. 
  4. ^ di Folco, E.; Absil, O.; Augereau, J.-C.; Mérand, A.; Coudé du Foresto, V.; Thévenin, F.; Defrère, D.; Kervella, P.; ten Brummelaar, T. A.; McAlister, H. A.; Ridgway, S. T.; Sturmann, J.; Sturmann, L.; Turner, N. H. (2007). "A near-infrared interferometric survey of debris disk stars". Astronomy and Astrophysics 475 (1): 243–250. arXiv:0710.1731. Bibcode:2007A&A...475..243D. doi:10.1051/0004-6361:20077625. 

External links[edit]