J/ApJ/893/56 T Tauri star IR excesses & Ha eq. widths (Manzo-Martinez+, 2020)
The evolution of the inner regions of protoplanetary disks.
Manzo-Martinez E., Calvet N., Hernandez J., Lizano S., Hernandez R.F.,
Miller C.J., Mauco K., Briceno C., D'Alessio P.
<Astrophys. J., 893, 56 (2020)>
=2020ApJ...893...56M 2020ApJ...893...56M
ADC_Keywords: Stars, pre-main sequence; Stars, masses; Spectral types;
Equivalent widths; Stars, distances; Infrared sources;
Star Forming Region
Keywords: Protoplanetary disks ; Pre-main sequence stars ; T Tauri stars ;
Stellar accretion disks
Abstract:
We present a study of the evolution of the inner few astronomical
units of protoplanetary disks around low-mass stars. We consider
nearby stellar groups with ages spanning from 1 to 11Myr, distributed
into four age bins. Combining PANSTARSS photometry with spectral
types, we derive the reddening consistently for each star, which we
use (1) to measure the excess emission above the photosphere with a
new indicator of IR excess and (2) to estimate the mass accretion rate
(dM/dt) from the equivalent width of the Hα line. Using the
observed decay of dM/dt as a constraint to fix the initial conditions
and the viscosity parameter of viscous evolutionary models, we use
approximate Bayesian modeling to infer the dust properties that
produce the observed decrease of the IR excess with age, in the range
between 4.5 and 24µm. We calculate an extensive grid of irradiated
disk models with a two-layered wall to emulate a curved dust inner
edge and obtain the vertical structure consistent with the surface
density predicted by viscous evolution. We find that the median dust
depletion in the disk upper layers is ε∼3x10-3 at 1.5Myr,
consistent with previous studies, and it decreases to
ε∼3x10-4 by 7.5Myr. We include photoevaporation in a simple
model of the disk evolution and find that a photoevaporative wind
mass-loss rate of ∼1-3x10-9M☉/yr agrees with the decrease of
the disk fraction with age reasonably well. The models show the inward
evolution of the H2O and CO snowlines.
Description:
To make a comprehensive statistical study of the evolution of disks
around T Tauri stars (TTSs), we selected nearby (≤500pc), young
(∼1 to 11Myr old) stellar groups with Spitzer photometry and with
available spectroscopic information for most of the TTSs reported in
each stellar group. The populations included in this work are:
the Orion Nebula Cluster (ONC), Taurus, the IC 348 cluster,
the σ Orionis cluster, the λ Orionis cluster,
the Orion OB1b sub-association, the Upper Scorpius sub-association
(UpSco), the γ Velorum cluster, and the Orion OB1a
sub-association, which includes the stellar aggregates 25 Ori,
HD35762, and HR 1833 (see Table 1).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 65 9 Stellar groups
table5.dat 129 835 Stellar properties
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See also:
II/349 : The Pan-STARRS release 1 (PS1) Survey - DR1 (Chambers+, 2016)
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
J/AJ/113/1733 : Orion Nebula Cluster population (Hillenbrand 1997)
J/AJ/124/404 : Upper Scorpius OB assoc. Lithium survey. II. (Preibisch, 2002)
J/ApJ/602/816 : Chamaeleon I star-forming region census (Luhman, 2004)
J/ApJ/651/L49 : Upper Sco OB association IRAC observations (Carpenter+, 2006)
J/AJ/131/1574 : Infrared photometry of IC348 members (Lada+, 2006)
J/ApJ/667/308 : Weak-line T Tauri in Spitzer c2d Survey. II. (Cieza+, 2007)
J/ApJ/671/1784 : Ori OB1 IRAC/MIPS observations (Hernandez+, 2007)
J/ApJ/662/1067 : Sptizer observations of sigma Orionis (Hernandez+, 2007)
J/A+A/492/277 : Analysis of Collinder 69 stars with VOSA (Bayo+, 2008)
J/ApJ/686/1195 : IR photometry in the γ Vel cluster (Hernandez+, 2008)
J/A+A/488/167 : Low-mass stars in σ Ori and λ Ori (Sacco+, 2008)
J/ApJ/698/1 : Spitzer observations of NGC 2362 (Currie+, 2009)
J/ApJ/703/1964 : Spectra of three nearby star-forming regions (Furlan+, 2009)
J/ApJ/722/1092 : Optical photometry of the ONC. II. (Da Rio+, 2010)
J/ApJ/722/1226 : IR photometry in λ Orionis cluster (Hernandez+, 2010)
J/ApJS/186/111 : Spitzer observations of Taurus members (Luhman+, 2010)
J/A+A/536/A63 : Collinder 69 very low mass stars & brown dwarfs (Bayo+, 2011)
J/ApJ/758/31 : IR photometry for members of Upper Sco (Luhman+, 2012)
J/AJ/144/192 : Spitzer survey of Orion A & B. I. YSO catalog (Megeath+, 2012)
J/ApJ/746/154 : Improved kinematic plx for Sco-Cen members (Pecaut+, 2012)
J/AJ/144/8 : Sp. of ∼100 G/K/M-type Sco-Cen complex members (Song+, 2012)
J/ApJ/750/99 : The Pan-STARRS1 photometric system (Tonry+, 2012)
J/AJ/146/85 : Spectral types of optical stars in ONC (Hillenbrand+, 2013)
J/ApJS/208/9 : Intrinsic colors and temperatures of PMS stars (Pecaut+, 2013)
J/A+A/561/A2 : 36 accreting YSOs emission lines (Alcala+, 2014)
J/ApJ/784/126 : IR photometry of all known members in Taurus (Esplin+, 2014)
J/ApJ/794/36 : σ Orionis cluster stellar population (Hernandez+, 2014)
J/A+A/567/A55 : Metallicity of the γ Vel cluster (Spina+, 2014)
J/A+A/575/A4 : Activity & accretion in γ Vel and Cha I (Frasca+, 2015)
J/A+A/589/A70 : Gamma Vel cluster membership and IMF (Prisinzano+, 2016)
J/A+A/589/A115 : Na and Al abundances of 1303 stars (Smiljanic+, 2016)
J/ApJ/847/31 : Protoplanetary disk data in Cha I and Lupus (Mulders+, 2017)
J/ApJ/869/L41 : DSHARP I. Sample, ALMA obs. log and overview (Andrews+, 2018)
J/MNRAS/477/L50 : Structure of the Upper Scorpius association (Galli+, 2018)
J/ApJ/863/13 : Herschel obs. of protoplanetary disks in L1641 (Grant+, 2018)
J/AJ/156/84 : APOGEE-2 survey of Orion Complex. II. (Kounkel+, 2018)
J/ApJ/865/73 : GOBELINS. V. Kinematics of Perseus (Ortiz-Leon+, 2018)
J/AJ/157/85 : The CIDA Variability Survey of Orion OB1. II. (Briceno+, 2019)
J/A+A/630/A137 : Structure and kinematics of the Taurus region (Galli+, 2019)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 12 A12 --- Group Stellar group
14- 16 I3 pc Dist1 Lower range of distance or mean distance
17 A1 --- --- [- ]
18- 20 I3 pc Dist2 ? Upper range of distance
22- 24 F3.1 Myr Age1 Lower range of age or mean age
25 A1 --- --- [- ]
26- 27 I2 Myr Age2 ? Upper age
29- 32 F4.1 % fdisk1 [5/73] Disk fraction (or lower range)
34- 35 I2 % fdisk2 [7/17]? Upper range of disk fraction
37- 41 F5.2 % e_fdisk [0.02/12]? Disk fraction uncertainty
43- 51 A9 --- Ref References (1)
53- 55 I3 --- Samp0 [59/508] Initial sample (2)
57- 59 I3 --- Ndk [13/305] Disk-bearing stars (3)
61- 63 I3 --- SampA [16/228]? Accretors sample (4)
65 I1 --- Bin [1/4] Age bin (5)
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Note (1): References as follows:
1 = Lada et al. (2006, J/AJ/131/1574)
2 = Hernandez et al. (2007, J/ApJ/662/1067)
3 = Hernandez et al. (2010, J/ApJ/722/1226)
4 = Briceno et al. (2019, J/AJ/157/85)
5 = Hernandez et al. (2008, J/ApJ/686/1195)
6 = Hernandez et al. (2007, J/ApJ/671/1784)
7 = Hillenbrand et al. (2013, J/AJ/146/85)
8 = Galli et al. (2019, J/A+A/630/A137)
9 = Luhman & Mamajek (2012, J/ApJ/758/31)
10 = Ortiz-Leon et al. (2018, J/ApJ/865/73)
11 = Perez-Blanco et al. (2018ApJ...867..116P 2018ApJ...867..116P)
12 = Kounkel et al. (2018, J/AJ/156/84)
13 = Galli et al. (2018, J/MNRAS/477/L50)
14 = David et al. (2019ApJ...872..161D 2019ApJ...872..161D)
15 = Franciosini et al. (2018A&A...616L..12F 2018A&A...616L..12F)
16 = Jeffries et al. (2017MNRAS.464.1456J 2017MNRAS.464.1456J)
* = Using the data from Luhman+ (2010, J/ApJS/186/111) we estimate a disk
fraction of 63.7±5.1 in Taurus.
Note (2): The number of K0-M6 stars initially compiled (diskless and
disk-bearing stars) with IRAC and PANSTARRS photometry in each stellar
group.
Note (3): The number of stars with near-IR excess above the photosphere,
separated according to Section 2.3, which correspond to the sample
used to study the dust component of the disks.
Note (4): The number of stars in the Classical TTSs (CTTSs)/accretors (CWTTSs)
sample, described in Section 2.6.1 used to study the evolution of dM/dt.
Note (5): Age bin (see Section 2.4) as follows:
1 = Bin 1 (1-2Myr): ONC and Taurus
2 = Bin 2 (2-3Myr): IC 348 and σ-Ori
3 = Bin 3 (3-5Myr): λ Ori, Ori OB1b, and Upper Sco
4 = Bin 4 (5-11Myr): γ Vel and Ori OB1a.
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 12 A12 --- Group Stellar group
14- 29 A16 --- 2MASS 2MASS source identifier
(HHMMSSss+DDMMSSs; J2000)
31- 35 A5 --- SpT Spectral Type
37- 40 F4.2 mag Av [0/9.1] Reddening, V band
42- 45 I4 K Teff [2600/5030] Stellar effective temperature
47- 48 I2 --- r_SpT [1/12] Reference for Spectral Type (1)
50- 53 F4.2 Lsun Lstar [0.01/5.8]? Stellar luminosity
55- 58 F4.2 Msun Mstar [0.01/1.7]? Stellar mass
60- 63 F4.2 Rsun Rstar [0.3/4.2]? Stellar radius
65- 69 F5.1 pc Dist [-1/790]? Distance
71- 76 F6.1 0.1nm EWHa [-400/-2.8]? Equivalent Width, Hα (2)
78- 82 F5.2 mag DCE(J-4.5) [-0.5/4.9]? Disk color excess, J-4.5um
84- 87 F4.2 mag e_DCE(J-4.5) [0.02/0.3]? Uncertainty in DCE(J-4.5) (3)
89- 93 F5.2 mag DCE(J-5.8) [-0.4/5.2]? Disk color excess, J-5.8um
95- 98 F4.2 mag e_DCE(J-5.8) [0.02/0.4]? Uncertainty in DCE(J-5.8) (3)
100-104 F5.2 mag DCE(J-8.0) [-0.6/6.2]? Disk color excess, J-8.0um
106-109 F4.2 mag e_DCE(J-8.0) [0.02/0.5]? Uncertainty in DCE(J-8.0) (3)
111-115 F5.2 mag DCE(J-24) [0.3/13.7]? Disk color excess, J-24um
117-120 F4.2 mag e_DCE(J-24) [0.02/0.9]? Uncertainty in DCE(J-24) (3)
122-129 E8.3 Msun/yr dM/dt [2.9e-11/5.4e-08]? Mass accretion Rate
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Note (1): References for Spectral Types as follows:
1 = Hernandez J. et al. (2020 in prep.; 299 occurrences)
2 = Briceno et al. (2019, J/AJ/157/85)
3 = Hillenbrand (1997, J/AJ/113/1733)
4 = Hillenbrand et al. (2013, J/AJ/146/85)
5 = Esplin et al. (2014, J/ApJ/784/126)
6 = Lada et al. (2006, J/AJ/131/1574)
7 = Hernandez et al. (2014, J/ApJ/794/36)
8 = Bayo et al. (2008, J/A+A/492/277)
9 = Bayo et al. (2011, J/A+A/536/A63)
10 = Luhman & Mamajek (2012, J/ApJ/758/31)
11 = Spina et al. (2014, J/A+A/567/A55)
12 = This work (8 occurrences)
Note (2): References for Equivalent width, Hα, by stellar group:
ONC = Hernandez J. et al. (2020 in prep.)
Taurus = this work
σ Ori = Hernandez et al. (2014, J/ApJ/794/36)
Ori OB1b = Briceno et al. (2019, J/AJ/157/85)
Ori OB1a = Briceno et al. (2019, J/AJ/157/85)
Note (3): The errors associated to the DCEs are based only on the photometric
errors and thus they are underestimated.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 08-Sep-2021