Extreme conditions in a close analog to the young solar system: Herschel observations of Eridani

Jane Sophia Greaves, B. Sibthorpe, B. Acke, E. E. Pantin, B. Vandenbussche, G. Olofsson, C. Dominik, M. J. Barlow, G. J. Bendo, J. A. D. L. 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. IvisonR. Liseau, B. C. Matthews, G. L. Pilbratt, H. J. Walker, C. Waelkens

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30 Citations (Scopus)


Far-infrared Herschel images of the Eridani system, seen at a fifth of the Sun's present age, resolve two belts of debris emission. Fits to the 160 μm PACS image yield radial spans for these belts of 12-16 and 54-68 AU. The south end of the outer belt is ≈10% brighter than the north end in the PACS+SPIRE images at 160, 250, and 350 μm, 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 (ec ≈ 0.03-0.3). Compared to the asteroid and Kuiper Belts of the young Sun, the 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 ≈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 Eri b, at semi-major axis ≈3 AU.

Original languageEnglish
Number of pages5
JournalAstrophysical Journal Letters
Issue number1
Early online date25 Jul 2014
Publication statusPublished - 10 Aug 2014


  • Circumstellar matter
  • Planet-disk interactions
  • Stars: individual (is an element of Eridani)
  • Star epison-eridani
  • Devris disk
  • Size distributions
  • Vega
  • Planets
  • Evolution
  • Migration
  • Spitzer
  • Belt
  • Mass


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