J/ApJ/709/L114 Protoplanetary disks in PMS binaries (Duchene, 2010)
Planet formation in binary systems: a separation-dependent mechanism?
Duchene G.
<Astrophys. J., 709, L114-L118 (2010)>
=2010ApJ...709L.114D 2010ApJ...709L.114D
ADC_Keywords: Photometry, millimetric/submm ; Planets ; YSOs ;
Stars, pre-main sequence ; Stars, double and multiple
Keywords: binaries: general - planetary systems -
planets and satellites: formation - protoplanetary disks
Abstract:
In this Letter, I examine several observational trends regarding
protoplanetary disks, debris disks, and exoplanets in binary systems
in an attempt to constrain the physical mechanisms of planet formation
in such a context. Binaries wider than about 100AU are
indistinguishable from single stars in all aspects. Binaries in the
5-100AU range, on the other hand, are associated with shorter lived
but (at least in some cases) equally massive disks. Furthermore, they
form planetesimals and mature planetary systems at a similar rate as
wider binaries and single stars, albeit with the peculiarity that they
predominantly produce high-mass planets. I posit that the location of
a stellar companion influences the relative importance of the core
accretion and disk fragmentation planet formation processes, with the
latter mechanism being predominant in binaries tighter than 100AU.
Description:
In order to draw a broad and homogeneous view of the initial
conditions for planet formation, I compiled a sample of 107 PMS
binaries for which deep (sub)millimeter continuum observations and/or
near- to mid-infrared colors are available in the literature (see
Table 1).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 86 107 Sample of Taurus and Ophiuchus protoplanetary
disks considered in this study
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See also:
J/ApJ/696/L84 : Primordial circumstellar disks in binary systems (Cieza+,
2009)
J/ApJ/703/1964 : Spectra of three nearby star-forming regions (Furlan+, 2009)
J/PASJ/60/209 : Faint companions around YSOs in TMC (Itoh+, 2008)
J/ApJS/179/451 : Predicted IR excesses for protoplanetary disks (Kenyon+, 2008)
J/ApJ/671/1800 : SCUBA observations of ρ Oph cloud (Andrews+, 2007)
J/ApJ/647/1180 : Infrared photometry of Taurus SFR (Luhman+, 2006)
J/ApJ/636/932 : Mid-infrared survey of T Tauri stars (McCabe+, 2006)
J/A+A/372/173 : ISOCAM observations of the rho Ophiuchi cloud (Bontemps+,
2001)
J/ApJS/101/117 : UBVRIJHKLMNQ photometry in Taurus-Auriga (Kenyon+ 1995)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 13 A13 --- Region Region (Taurus-Auriga or Ophiucius)
15- 34 A20 --- Target Target name (Pre-Main-Sequence star)
36- 46 A11 --- AName Alternate target name
48- 53 F6.1 AU Sep Separation between the stars
55- 59 F5.2 mag Color ? Spitzer/IRAC 3.6-8.0 micron band color index
61 A1 --- f_Color [cdegh] reason of missing Color (1)
63 A1 --- d? [Y/N] Inner disk present?
65 A1 --- f_d? [f] Presence of inner disk from SED (2)
67 A1 --- l_F.85 Limit on F.85
68- 73 F6.1 mJy F.85 ? Flux density at 850 micron
75 A1 --- l_F1.3 Limit on F1.3
76- 80 F5.1 mJy F1.3 ? Flux density at 1.3mm
82- 86 A5 --- Ref Reference(s) (3)
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Note (1): Flag as follows:
c = In the absence of a 3.6 micron measurement, I used the [4.5]-[8.0]
color and assumed that [3.6]-[8.0] ≥ [4.5]-[8.0].
d = In the absence of published Spitzer/IRAC photometry of the system,
I used the K-N color.
e = In the absence of published Spitzer/IRAC photometry of the system,
I used the K-L color.
g = In the absence of published Spitzer/IRAC photometry of the system,
I used the L-N color and assumed that K-N ≥ L-N.
h = In the absence of published Spitzer/IRAC photometry of the system,
I used the α_2-14 micron_ spectral index.
Note (2):
f = In the absence of published infrared photometry beyond 3 micron,
I relied on the "SED class" from Andrews & Williams
(2005ApJ...631.1134A 2005ApJ...631.1134A, 2007, Cat. J/ApJ/671/1800).
For Taurus sources, this classification is based on the classification
proposed by Kenyon & Hartmann (1995, Cat. J/ApJS/101/117).
Note (3): References as follows:
1 = Luhman et al.(2006, Cat. J/ApJ/647/1180);
2 = Andrews & Williams (2005ApJ...631.1134A 2005ApJ...631.1134A);
3 = Hartmann et al.(2005ApJ...629..881H 2005ApJ...629..881H);
4 = Cieza et al.(2009, Cat. J/ApJ/696/L84);
5 = McCabe et al.(2006, Cat. J/ApJ/636/932);
6 = Guilloteau et al.(1999A&A...348..570G 1999A&A...348..570G);
7 = Kenyon & Hartmann (1995, Cat. J/ApJS/101/117);
8 = Duchene et al.(2010ApJ...712..112D 2010ApJ...712..112D);
9 = Jensen & Akeson (2003ApJ...584..875J 2003ApJ...584..875J);
10 = Jensen et al.(1996ApJ...458..312J 1996ApJ...458..312J);
11 = Andrews & Williams (2007, Cat. J/ApJ/671/1800);
12 = Bontemps et al. (2001, Cat. J/A+A/372/173).
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 09-Mar-2012