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. Ivison; R. Liseau; B. C. Matthews; G. L. Pilbratt; H. J. Walker; C. Waelkens

doi:10.1088/2041-8205/791/1/L11

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

School of Physics and Astronomy

Research output: Contribution to journal › Article › peer-review

Abstract

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 (e_c ≈ 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 language	English
Number of pages	5
Journal	Astrophysical Journal Letters
Volume	791
Issue number	1
Early online date	25 Jul 2014
DOIs	https://doi.org/10.1088/2041-8205/791/1/L11
Publication status	Published - 10 Aug 2014

Keywords

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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10.1088/2041-8205/791/1/L11

Greaves_2014_TAJT_Extreme
Copyright 2014. The American Astronomical Society. All rights reserved. This work is made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at http://dx.doi.org/10.1088/2041-8205/791/1/L11
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Astrophysics at St Andrews:2012 - 2014: Astrophysics at St Andrews: 2012 - 2014
Horne, K. D. (PI)
Science & Technology Facilities Council
1/10/11 → 31/03/12
Project: Standard

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Greaves, J. S., Sibthorpe, B., Acke, B., Pantin, E. E., Vandenbussche, B., Olofsson, G., Dominik, C., Barlow, M. J., Bendo, G. J., Blommaert, J. A. D. L., Brandeker, A., de Vries, B. L., Dent, W. R. F., Di Francesco, J., Fridlund, M., Gear, W. K., Harvey, P. M., Hogerheijde, M. R., Holland, W. S., ... Waelkens, C. (2014). Extreme conditions in a close analog to the young solar system: Herschel observations of _∈ Eridani. Astrophysical Journal Letters, 791(1). https://doi.org/10.1088/2041-8205/791/1/L11

@article{e383ee1520e549a090ee90ada38f0a6f,

title = "Extreme conditions in a close analog to the young solar system: Herschel observations of ∈ Eridani",

abstract = "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.",

keywords = "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",

author = "Greaves, {Jane Sophia} and B. Sibthorpe and B. Acke and Pantin, {E. E.} and B. Vandenbussche and G. Olofsson and C. Dominik and Barlow, {M. J.} and Bendo, {G. J.} and Blommaert, {J. A. D. L.} and A. Brandeker and {de Vries}, {B. L.} and Dent, {W. R. F.} and {Di Francesco}, J. and M. Fridlund and Gear, {W. K.} and Harvey, {P. M.} and Hogerheijde, {M. R.} and Holland, {W. S.} and Ivison, {R. J.} and R. Liseau and Matthews, {B. C.} and Pilbratt, {G. L.} and Walker, {H. J.} and C. Waelkens",

year = "2014",

month = aug,

day = "10",

doi = "10.1088/2041-8205/791/1/L11",

language = "English",

volume = "791",

journal = "Astrophysical Journal Letters",

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publisher = "American Astronomical Society",

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Greaves, JS, Sibthorpe, B, Acke, B, Pantin, EE, Vandenbussche, B, Olofsson, G, Dominik, C, Barlow, MJ, Bendo, GJ, Blommaert, JADL, Brandeker, A, de Vries, BL, Dent, WRF, Di Francesco, J, Fridlund, M, Gear, WK, Harvey, PM, Hogerheijde, MR, Holland, WS, Ivison, RJ, Liseau, R, Matthews, BC, Pilbratt, GL, Walker, HJ & Waelkens, C 2014, 'Extreme conditions in a close analog to the young solar system: Herschel observations of _∈ Eridani', Astrophysical Journal Letters, vol. 791, no. 1. https://doi.org/10.1088/2041-8205/791/1/L11

TY - JOUR

T1 - Extreme conditions in a close analog to the young solar system

T2 - Herschel observations of ∈ Eridani

AU - Greaves, Jane Sophia

AU - Sibthorpe, B.

AU - Acke, B.

AU - Pantin, E. E.

AU - Vandenbussche, B.

AU - Olofsson, G.

AU - Dominik, C.

AU - Barlow, M. J.

AU - Bendo, G. J.

AU - Blommaert, J. A. D. L.

AU - Brandeker, A.

AU - de Vries, B. L.

AU - Dent, W. R. F.

AU - Di Francesco, J.

AU - Fridlund, M.

AU - Gear, W. K.

AU - Harvey, P. M.

AU - Hogerheijde, M. R.

AU - Holland, W. S.

AU - Ivison, R. J.

AU - Liseau, R.

AU - Matthews, B. C.

AU - Pilbratt, G. L.

AU - Walker, H. J.

AU - Waelkens, C.

PY - 2014/8/10

Y1 - 2014/8/10

N2 - 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.

AB - 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.

KW - Circumstellar matter

KW - Planet-disk interactions

KW - Stars: individual (is an element of Eridani)

KW - Star epison-eridani

KW - Devris disk

KW - Size distributions

KW - Vega

KW - Planets

KW - Evolution

KW - Migration

KW - Spitzer

KW - Belt

KW - Mass

U2 - 10.1088/2041-8205/791/1/L11

DO - 10.1088/2041-8205/791/1/L11

M3 - Article

SN - 2041-8205

VL - 791

JO - Astrophysical Journal Letters

JF - Astrophysical Journal Letters

IS - 1

ER -

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

Abstract

Keywords

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Astrophysics at St Andrews:2012 - 2014: Astrophysics at St Andrews: 2012 - 2014

Cite this

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