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Extreme Conditions in a Close Analog to the Young Solar System: Herschel Observations of ∈ Eridani

J. S. Greaves ; B. Sibthorpe ; B. Acke ; E. E. Pantin ; B. Vandenbussche ; G. Olofsson ; C. Dominik ; M. J. Barlow ; G. J. Bendo ; Jadl Blommaert ; A. Brandeker ; B. L. de Vries ; W. R. F. Dent ; J. Di Francesco ; M. Fridlund ; W. K. Gear ; P. M. Harvey ; M. R. Hogerheijde ; W. S. Holland ; R. J. Ivison ; René Liseau (Institutionen för rymd- och geovetenskap, Radioastronomi och astrofysik) ; B. C. Matthews ; G. L. Pilbratt ; H. J. Walker ; C. Waelkens
Astrophysical Journal Letters (2041-8205). Vol. 791 (2014), 1,
[Artikel, refereegranskad vetenskaplig]

Far-infrared Herschel images of the is an element of Eridani system, seen at a fifth of the Sun's present age, resolve two belts of debris emission. Fits to the 160 mu m PACS image yield radial spans for these belts of 12-16 and 54-68 AU. The south end of the outer belt is approximate to 10% brighter than the north end in the PACS+SPIRE images at 160, 250, and 350 mu m, indicating a pericenter glow attributable to a planet "c" From this asymmetry and an upper bound on the offset of the belt center, this second planet should be mildly eccentric (e(c) approximate to 0.03-0.3). Compared to the asteroid and Kuiper Belts of the young Sun, the is an element of Eri belts are intermediate in brightness and more similar to each other, with up to 20 km sized collisional fragments in the inner belt totaling approximate to 5% of an Earth mass. This reservoir may feed the hot dust close to the star and could send many impactors through the Habitable Zone, especially if it is being perturbed by the suspected planet is an element of Eri b, at semi-major axis approximate to 3 AU.

Nyckelord: circumstellar matter, planet-disk interactions, stars: individual (is an element of Eridani), STAR EPSILON-ERIDANI, DEBRIS DISK, SIZE DISTRIBUTIONS, VEGA, PLANETS, EVOLUTION, MIGRATION, SPITZER, BELT, MASS



Denna post skapades 2014-11-10. Senast ändrad 2014-11-10.
CPL Pubid: 205493

 

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