2010MNRAS.404.1944G


Query : 2010MNRAS.404.1944G

2010MNRAS.404.1944G - Mon. Not. R. Astron. Soc., 404, 1944-1951 (2010/June-1)

Debris discs and comet populations around Sun-like stars: the solar system in context.

GREAVES J.S. and WYATT M.C.

Abstract (from CDS):

Numerous nearby FGK dwarfs possess discs of debris generated by collisions among comets. Here, we fit the levels of dusty excess observed by Spitzer at 70µm and show that they form a rather smooth distribution. Taking into account the transition of the dust removal process from collisional to Poynting-Robertson drag, all the stars may be empirically fitted by a single population with many low-excess members. Within this ensemble, the Kuiper Belt is inferred to be such a low-dust example, among the last 10 per cent of stars, with a small cometary population. Analogue systems hosting gas giant planets and a modest comet belt should occur for only a few per cent of Sun-like stars, and so terrestrial planets with a comparable cometary impact rate to the Earth may be uncommon. The nearest such analogue system presently known is HD 154345 at 18pc, but accounting for survey completeness, a closer example should lie at around 10pc.

Abstract Copyright: © 2010 The Authors. Journal compilation © 2010 RAS

Journal keyword(s): circumstellar matter - planetary systems - infrared: stars

Simbad objects: 11

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Number of rows : 11
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026
#notes
1 * q01 Eri PM* 01 42 29.3145176952 -53 44 26.991453264   6.05 5.52     F9V 368 1
2 * tau Cet PM* 01 44 04.0831371922 -15 56 14.927607677 4.43 4.22 3.50 2.88 2.41 G8V 1354 1
3 * 58 Eri BY* 04 47 36.2917029384 -16 56 04.040472552   6.14 5.50     G2.5IV-V 466 0
4 * pi. Men PM* 05 37 09.8868446714 -80 28 08.834553264   6.25 5.67     G0V 390 1
5 * psi05 Aur PM* 06 46 44.3369350032 +43 34 38.728429752       4.9   F9V 283 0
6 HD 69830 PM* 08 18 23.9469682407 -12 37 55.817187530   6.74 5.95     G8:V 587 1
7 NGC 2632 OpC 08 39 58.4 +19 36 33           ~ 1733 0
8 * g Lup PM* 15 41 11.3768069149 -44 39 40.341696305   5.036 4.633     F4V 212 0
9 * 18 Sco PM* 16 15 37.2702755653 -08 22 09.982125430   6.15 5.50     G2Va 671 0
10 HD 154345 PM* 17 02 36.4038090379 +47 04 54.764174452   7.50   6.3   G9 297 1
11 * alf PsA PM* 22 57 39.04625 -29 37 20.0533 1.31 1.25 1.16 1.11 1.09 A4V 1303 3

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