J/MNRAS/442/2543 Dust disks around star in young clusters (Yasui+, 2014)
Rapid evolution of the innermost dust disc of protoplanetary discs surrounding
intermediate-mass stars.
Yasui C., Kobayashi N., Tokunaga A.T., Saito M.
<Mon. Not. R. Astron. Soc., 442, 2543-2559 (2014)>
=2014MNRAS.442.2543Y 2014MNRAS.442.2543Y
ADC_Keywords: Associations, stellar ; MK spectral classification
Keywords: planets and satellites: formation - protoplanetary discs -
circumstellar matter - stars: pre main-sequence -
stars: variables: T Tauri, Herbig Ae/Be - infrared: stars
Abstract:
We derived the intermediate-mass (≃1.5-7M☉) disc fraction
(IMDF) in the near-infrared JHK photometric bands as well as in the
mid-infrared (MIR) bands for young clusters in the age range of 0 to
∼10Myr. From the JHK IMDF, the lifetime of the innermost dust disc
(∼0.3au; hereafter the K disc) is estimated to be ∼3Myr, suggesting a
stellar mass (M*) dependence of K-disc lifetime (≃1.5-7M☉).
However, from the MIR IMDF, the lifetime of the inner disc (∼5au;
hereafter the MIR disc) is estimated to be ∼6.5Myr, suggesting a very
weak stellar mass dependence (M*). The much shorter K-disc lifetime
compared to the MIR-disc lifetime for intermediate-mass (IM) stars
suggests that IM stars with transition discs, which have only MIR
excess emission but no K-band excess emission, are more common than
classical Herbig Ae/Be stars, which exhibit both. We suggest that this
prominent early disappearance of the K disc for IM stars is due to
dust settling/growth in the protoplanetary disc, and it could be one
of the major reasons for the paucity of close-in planets around IM
stars.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 80 19 Summary of target clusters
appen.dat 106 833 List of sample intermediate-mass stars in
target clusters
appendix.pdf 512 428 List of sample stars tables as well as
colour-colour diagrams
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Seq [1/19] Sequential number
4- 14 A11 --- Cluster Cluster name
16- 19 F4.1 Myr Age [1/11] Adopted age
21- 23 F3.1 Myr e_Age [0.5/3] rms uncertainty on Age
25- 29 A5 --- r_Age Reference for Age (1)
30- 33 I4 pc Dist [100/1500] Distance
35- 39 A5 --- r_Dist Reference for Dist (1)
41- 80 A40 --- Refs References for the disc fraction study in
the past (1) (2)
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Note (2): Note that some references show different cluster names (e.g. 25 Ori,
which is named as Ori OB1a in our list).
Note (1): References as follows:
Br05 = Briceno et al. (2005AJ....129..907B 2005AJ....129..907B, Cat. J/AJ/129/907)
Da08a = Dahm (2008HSFR1.B....966D 2008HSFR1.B....966D)
Da08b = Dahm (2008HSFR2.B.....26D 2008HSFR2.B.....26D)
El78 = Elias (1978ApJ...224..857E 1978ApJ...224..857E)
Fe10 = Fedele et al. (2010A&A...510A..72F 2010A&A...510A..72F)
Ga09 = Gaspar et al. (2009ApJ...697.1578G 2009ApJ...697.1578G, Cat. J/ApJ/697/1578)
Ha01a = Haisch et al. (2001AJ....121.2065H 2001AJ....121.2065H)
Ha01b = Haisch et al. (2001ApJ...553L.153H 2001ApJ...553L.153H)
He05 = Hernandez et al. (2005AJ....129..856H 2005AJ....129..856H, Cat. J/AJ/129/856)
He07a = Hernandez et al. (2007ApJ...662.1067H 2007ApJ...662.1067H, Cat. J/ApJ/662/1067)
He08 = Hernandez et al. (2008ApJ...686.1195H 2008ApJ...686.1195H, Cat. J/ApJ/686/1195)
He09 = Hernandez et al. (2009ApJ...707..705H 2009ApJ...707..705H)
Ke09 = Kennedy & Kenyon (2009ApJ...695.1210K 2009ApJ...695.1210K)
LL03 = Lada & Lada (2003ARA&A..41...57L 2003ARA&A..41...57L)
Lu08 = Luhman (2008ApJ...675.1375L 2008ApJ...675.1375L, Cat. J/ApJ/675/1375)
Ma09 = Mamajek (2009, AIP Conf. Proc. Vol. 1158, 3)
Ma99 = Mamajek, Lawson & Feigelson (1999ApJ...516L..77M 1999ApJ...516L..77M)
Mu02 = Muench et al. (2002ApJ...573..366M 2002ApJ...573..366M, Cat. J/ApJ/573/366)
Pr02 = Preibisch et al. (2002AJ....124..404P 2002AJ....124..404P, Cat. J/AJ/124/404)
Ro11 = Roccatagliata et al. (2011ApJ...733..113R 2011ApJ...733..113R, Cat. J/ApJ/733/113)
Si05 = Sicilia-Aguilar et al. (2005AJ....130..188S 2005AJ....130..188S, Cat. J/AJ/130/188)
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Byte-by-byte Description of file: appen.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Cluster Cluster name
12 A1 --- n_Name [*] Star with measured dynamical mass (1)
13- 36 A24 --- Name Star Name
37- 46 A10 --- OName Other Name
47 A1 --- fp [*] Position added at CDS (2)
48- 49 I2 h RAh Right ascension (J2000)
51- 52 I2 min RAm Right ascension (J2000)
54- 61 F8.5 s RAs Right ascension (J2000)
63 A1 --- DE- Declination sign (J2000)
64- 65 I2 deg DEd Declination (J2000)
67- 68 I2 arcmin DEm Declination (J2000)
70- 76 F7.4 arcsec DEs Declination (J2000)
78- 92 A15 --- SpType Spectral type in the literature
94 A1 --- r_SpType [*bw] iOrigin of the spectral type (3)
96 A1 --- Kd [Xo-] K-band disk (4)
98 A1 --- Md [Xo-] MIR disk (4)
99 A1 --- n_Md [+*] Note on Md for Taurus cluster (5)
100 A1 --- --- [(]
101-105 F5.2 --- alpha [-3.1/1.1]? SED slope α
= dlnλFλ/dlnλ
106 A1 --- --- [)]
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Note (1): Iin the Taurus cluster, the sample includes two low-mass stars
with measured dynamical masses: LkCa 15 (Hillenbrand & White
2004ApJ...604..741H 2004ApJ...604..741H; 0.84M☉) and V807 Tau (Schaefer et al.
2006AJ....132.2618S 2006AJ....132.2618S; 1.15M☉). By our criteria, both objects have
spectral type of K5 and are classified as IM stars. The dynamical mass of
V807 Tau is almost within the mass uncertainty of our method as described
in section 2.2. LkCa 15 has an estimated age (3-5Myr; Simon et al.,
2000ApJ...545.1034S 2000ApJ...545.1034S) that is much higher than the average Taurus cluster
age (1.5Myr; see also Fig. 3 in Simon et al., 2000ApJ...545.1034S 2000ApJ...545.1034S), which
we employed for our Intermediate-Mass star selection (see Sect. 2.2 and
Sect. 8.1.2). However, these stars are included for consistency with the
other clusters. As discussed in section 2.2 up to 15% of our sample of
Intermediate-Mass stars could be low mass stars.
Note (2): * indicates positions added by CDS from Simbad.
In original tables, only coordinates (in J2000) are shown if the object
names are not available in the references.
Note (3): the marks have the following meaning:
* = spectral type from SIMBAD database.
w = form BA92W94, Bouvier & Appenzeller, 1992A&AS...92..481B 1992A&AS...92..481B and
Wood et al., 1994ApJ...420..837A 1994ApJ...420..837A
b = from BA92, Bouvier & Appenzeller, 1992A&AS...92..481B 1992A&AS...92..481B
Note (4):
* The "Kd" and "Md" columns show objects with a disk (o) and
without a disk (X) in the K-band amd Mid-IR respectively.
* The stars with K-disk emission are judged from the colour-colour diagram,
(in appendix.pdf), in which the red and black circles show those with a
K disk and without a K disk, respectively.
* For ρ Oph cloud: because we could not find published IRAC photometry
data, we directly used the MIR disk classification in Wilking et al.
(2008HSFR2.B....351W 2008HSFR2.B....351W).
Note (5): for Taurus, flag as follows:
+ = marks show the members that are identified as having a disk from SEDs
in Furlan et al. (2006ApJS..165..568F 2006ApJS..165..568F),
* = marks show the members that are identified as without a disk from SEDs
in Furlan et al. (2011ApJS..195....3F 2011ApJS..195....3F)
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 04-Mar-2015