2002ApJ...578L.149Q

Query : 2002ApJ...578L.149Q

2002ApJ...578L.149Q - Astrophys. J., 578, L149-L152 (2002/October-3)

Structure in the ε eridani dusty disk caused by mean motion resonances with a 0.3 eccentricity planet at periastron.

QUILLEN A.C. and THORNDIKE S.

Abstract (from CDS):

The morphology of the ε Eridani dust ring is reproduced by a numerical simulation of dust particles captured into the 5:3 and 3:2 exterior mean motion resonances with a 0.3 eccentricity 10–4 M☉planet at periastron at a semimajor axis of 40 AU. The morphology will differ when the planet is at apastron, in about 140 yr. Moderate eccentricity planets in outer extrasolar systems will cause observable variations in the morphology of associated dusty rings.

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Journal keyword(s): Stars: Circumstellar Matter - Stars: Planetary Systems - Stars: Individual: Constellation Name: ε Eridani

Simbad objects: 6

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Number of rows : 6
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024 		#notes
1 * eps Eri BY* 03 32 55.8444911587 -09 27 29.739493865 5.19 4.61 3.73 3.00 2.54 K2V 1932 1
2 * eps Eri b Pl 03 32 55.8444911587 -09 27 29.739493865           ~ 146 1
3 * bet Pic PM* 05 47 17.0876901 -51 03 59.441135 4.13 4.03 3.86 3.74 3.58 A6V 1905 1
4 HD 109573 PM* 12 36 01.0317461592 -39 52 10.220465388   5.786 5.774 7.25 5.81 A0V 634 1
5 * alf Lyr dS* 18 36 56.33635 +38 47 01.2802 0.03 0.03 0.03 0.07 0.10 A0Va 2687 1
6 * alf PsA PM* 22 57 39.04625 -29 37 20.0533 1.31 1.25 1.16 1.11 1.09 A4V 1236 3

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