2004ApJ...612L..73L

Query : 2004ApJ...612L..73L

2004ApJ...612L..73L - Astrophys. J., 612, L73-L76 (2004/September-1)

The core accretion model predicts few Jovian-mass planets orbiting red dwarfs.

LAUGHLIN G., BODENHEIMER P. and ADAMS F.C.

Abstract (from CDS):

The favored theoretical explanation for giant planet formation–in both our solar system and others–is the core accretion model (although it still has some serious difficulties). In this scenario, planetesimals accumulate to build up planetary cores, which then accrete nebular gas. With current opacity estimates for protoplanetary envelopes, this model predicts the formation of Jupiter-mass planets in 2-3 Myr at 5 AU around solar-mass stars, provided that the surface density of solids is enhanced over that of the minimum-mass solar nebula (by a factor of a few). Working within the core accretion paradigm, this Letter presents theoretical calculations that show that the formation of Jupiter-mass planets orbiting M dwarf stars is seriously inhibited at all radial locations (in sharp contrast to solar-type stars). Planet detection programs sensitive to companions of M dwarfs will test this prediction in the near future.

Abstract Copyright: ∼

Journal keyword(s): Stars: Planetary Systems: Formation - Stars: Planetary Systems: Protoplanetary Disks - Stars: Formation

Simbad objects: 1

Full paper

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Number of rows : 1

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	BD-15 6290	BY*	22 53 16.7325836486	-14 15 49.304052185	12.928	11.749	10.192	9.013	7.462	M3.5V	1106	1

Query : 2004ApJ...612L..73L

Basic data :

BD-15 6290 -- BY Dra Variable

* (2015ApJS,BD,...), PM* (2013MNRAS,Ci,...), BY* (2017ARep), Ro* (2012A&A), V* (V*), NIR (2MASS), MIR (WISEA)

22 53 16.7325836486 -14 15 49.304052185 (Optical) [ 0.0338 0.0258 90 ] A 2020yCat.1350....0G

22 50 34.6499284991 -14 31 14.052098435 [ 0.0338 0.0258 90 ]

052.0040597500243 -59.6300891766021 [ 0.0338 0.0258 90 ]

957.715 -673.601 [0.041 0.031 90] A 2020yCat.1350....0G

V(km/s) -1.47 [0.0003] / z(spectroscopic) -0.000005 [0.000000] / cz -1.47 [0.00] (Opt) A 2018MNRAS.475.1960F

214.0380 [0.0356] A 2020yCat.1350....0G

M3.5V C 1983SAAOC...7..106W

U 12.928 [0.0034] B 2009AJ....137.4186L

B 11.749 [0.0017] B 2009AJ....137.4186L

V 10.192 [0.0017] B 2009AJ....137.4186L

R 9.013 [0.0017] B 2009AJ....137.4186L

G 8.875059 [0.002861] C 2020yCat.1350....0G

I 7.462 [0.0017] B 2009AJ....137.4186L

J 5.934 [0.019] C 2003yCat.2246....0C

H 5.349 [0.049] C 2003yCat.2246....0C

K 5.010 [0.021] C 2003yCat.2246....0C

g 10.919 [~] D 2012yCat.1322....0Z

r 9.872 [0.08] D 2012yCat.1322....0Z

i 8.296 [0.05] D 2012yCat.1322....0Z

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`BD-15 6290`	`GSC 05819-00957`	`NAME NC 59`	`UBV M 5470`
`Ci 20 1387`	`HIC 113020`	`NLTT 55130`	`UCAC2 26801725`
`CNS5 5644`	`HIP 113020`	`8pc 212.69A`	`UCAC4 379-165686`
`EPIC 206019387`	`JP11 295`	`PLX 5546`	*`V IL Aqr`**
`EPIC 206019392`	`Karmn J22532-142`	`PLX 5546.00`	`WEB 20121`
`GCRV 14365`	`LFT 1745`	`PM J22532-1415`	`WISEA J225317.42-141556.1`
`GEN# -0.01506290`	`LHS 530`	`Ross 780`	`Zkh 338`
`G 156-57A`	`LPM 841`	`TIC 188580272`	`[RHG95] 3604`
`G 156-57`	`LTT 9244`	`TYC 5819-1255-1`	`Gaia DR3 2603090003484152064`
`GJ 876`	`2MASS J22531672-1415489`	`UBV 19209`	`Gaia DR2 2603090003484152064`
`GJ 876 A`	`MCC 337`	`UBV 19610`

References (1106 between 1850 and 2026) (Total 1106)
Simbad bibliographic survey began in 1850 for stars (at least bright stars) and in 1983 for all other objects (outside the solar system).

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`BD-15 6290`	`G 156-57A`	`G 156-57`	`GJ 876`	`GJ 876 A`
`GSC 05819-00957`	`HIC 113020`	`HIP 113020`	`LHS 530`	`2MASS J22531672-1415489`
`NLTT 55130`	`PLX 5546`	`TYC 5819-1255-1`	`UCAC2 26801725`	`UCAC4 379-165686`
*`V IL Aqr`**	`WISEA J225317.42-141556.1`	`Gaia DR3 2603090003484152064`	`Gaia DR2 2603090003484152064`

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