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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
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:

       FileName      Lrecl  Records   Explanations

ReadMe            80        .   This file
table1.dat        86      107   Sample of Taurus and Ophiuchus protoplanetary
                             disks considered in this study


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

   Bytes Format Units   Label     Explanations

   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)

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, 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);
    3 = Hartmann et al.(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);
    7 = Kenyon & Hartmann (1995, Cat. J/ApJS/101/117);
    8 = Duchene et al.(2010ApJ...712..112D);
    9 = Jensen & Akeson (2003ApJ...584..875J);
   10 = Jensen et al.(1996ApJ...458..312J);
   11 = Andrews & Williams (2007, Cat. J/ApJ/671/1800);
   12 = Bontemps et al. (2001, Cat. J/A+A/372/173).


History:
    From electronic version of the journal
(End)                 Greg Schwarz [AAS], Emmanuelle Perret [CDS]    09-Mar-2012