J/ApJ/847/31 Protoplanetary disk data in Cha I and Lupus (Mulders+, 2017)
Constraints from dust mass and mass accretion rate measurements on angular
momentum transport in protoplanetary disks.
Mulders G.D., Pascucci I., Manara C.F., Testi L., Herczeg G.J., Henning T.,
Mohanty S., Lodato G.
<Astrophys. J., 847, 31 (2017)>
=2017ApJ...847...31M 2017ApJ...847...31M
ADC_Keywords: Accretion; Stars, masses; Spectral types; YSOs; Molecular clouds
Keywords: accretion, accretion disks ; planets and satellites: formation ;
protoplanetary disks ; stars: low-mass
Abstract:
In this paper, we investigate the relation between disk mass and mass
accretion rate to constrain the mechanism of angular momentum
transport in protoplanetary disks. We find a correlation between dust
disk mass and mass accretion rate in Chamaeleon I with a slope that is
close to linear, similar to the one recently identified in Lupus. We
investigate the effect of stellar mass and find that the intrinsic
scatter around the best-fit Mdust-M* and dMacc/dt-M* relations
is uncorrelated. We simulate synthetic observations of an ensemble of
evolving disks using a Monte Carlo approach and find that disks with a
constant α viscosity can fit the observed relations between dust
mass, mass accretion rate, and stellar mass but overpredict the
strength of the correlation between disk mass and mass accretion rate
when using standard initial conditions. We find two possible
solutions. In the first one, the observed scatter in Mdust and
dMacc/dt is not primordial, but arises from additional physical
processes or uncertainties in estimating the disk gas mass. Most
likely grain growth and radial drift affect the observable dust mass,
while variability on large timescales affects the mass accretion
rates. In the second scenario, the observed scatter is primordial, but
disks have not evolved substantially at the age of Lupus and
Chamaeleon I owing to a low viscosity or a large initial disk radius.
More accurate estimates of the disk mass and gas disk sizes in a large
sample of protoplanetary disks, through either direct observations of
the gas or spatially resolved multiwavelength observations of the dust
with ALMA, are needed to discriminate between both scenarios or to
constrain alternative angular momentum transport mechanisms such as
MHD disk winds.
Description:
We perform a homogeneous analysis of the dust disk mass, mass
accretion rate, and stellar mass in the Chamaeleon I and Lupus
star-forming regions. All observational data used in this analysis
were previously published; the ALMA data surveys of disk masses were
presented by Ansdell+ (2016, J/ApJ/828/46) and Pascucci+ (2016,
J/ApJ/831/125); the X-Shooter surveys of mass accretion rates were
presented by Alcala+ (2014, J/A+A/561/A2 ; 2017, J/A+A/600/A20) and
Manara+ (2014A&A...568A..18M 2014A&A...568A..18M ; 2016A&A...585A.136M 2016A&A...585A.136M and
2017, arXiv:1704.02842).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 119 174 Stellar and disk properties for Chamaeleon I and Lupus
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See also:
J/A+A/452/245 : Near-IR photometry of PMS stars in rho Oph (Natta+, 2006)
J/A+A/504/461 : YSOs in L1630N and L1641 (Fang+, 2009)
J/ApJ/710/597 : Accretion in disks in Cep OB2 (Sicilia-Aguilar+, 2010)
J/ApJ/771/129 : Submillimetric Class II sources of Taurus (Andrews+, 2013)
J/ApJS/207/5 : YSOs in LDN 1641 with Hectochelle spectra (Fang+, 2013)
J/A+A/561/A2 : 36 accreting YSOs emission lines (Alcala+, 2014)
J/A+A/570/A82 : Mapping accretion variability in NGC 2264 (Venuti+, 2014)
J/ApJ/814/130 : Planet occurrence rates calculated for KOIs (Mulders+, 2015)
J/A+A/581/A66 : UV variability and accretion in NGC 2264 (Venuti+, 2015)
J/ApJ/828/46 : ALMA survey of Lupus protoplanetary disks. I. (Ansdell+, 2016)
J/ApJ/831/125 : ALMA 887um obs. of ChaI star-forming region (Pascucci+, 2016)
J/A+A/592/A49 : TW Hya CO(2-1), CN(2-1) and CS(5-4) data cubes (Teague+, 2016)
J/A+A/600/A20 : Lupus YSOs X-shooter spectroscopy (Alcala+, 2017)
J/ApJ/841/116 : Herschel spectra of 11 very low mass stars (Hendler+, 2017)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 23 A23 --- ID Identifier, 2MASS J or other star name
25- 29 A5 --- SpT MK spectral type
31- 34 I4 K Teff [0/5110]? Stellar effective temperature
36- 40 F5.2 [Lsun] logL [-2.7/0.8]? log of stellar luminosity
42- 46 F5.2 [Rsun] logR [-0.9/0.6]? log of stellar radius
48- 52 F5.2 [Msun] logM [-1.6/0.3]? log of stellar mass
54- 57 F4.2 [Msun] e_logM [0.04/0.4]? Uncertainty in logM
59- 64 F6.2 [Lsun] logLacc [-5.3/0.7]? Log of accretion luminosity
66- 70 F5.2 [Mgeo] logMdust [-0.9/2.7]? Log of dust mass
72- 77 F6.4 [Mgeo] e_logMdust [0.0003/0.2]? Uncertainty in logMdust
79- 83 A5 --- Det [True /False] Source is detected in dust
continuum emission (>3σ)
85- 91 F7.2 [Msun/yr] logMacc [-12.3/-6.6]? log of mass accretion rate
93- 96 F4.2 [Msun/yr] e_logMacc [0.2/0.5] Uncertainty in logMacc
98-102 A5 --- Det2 [True /False] Accretion luminosity
> expected chromospheric emission
104-109 A6 --- Reg Region: Chamaeleon I (ChaI) or Lupus
111-119 A9 --- Exc Exclude? (1)
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Note (1): Reason why sources are not included in analysis as follows:
underlum = sub-luminous, lying below the ZAMS on HR diagram or
known edge-on disk (9 occurrences);
binary = apparent binary (1 occurrence);
faint = source not detected with VLT/X-shooter (4 occurrences);
noMdust = no dust mass measurement (14 occurrences);
notinslit = source not in VLT/X-shooter slit (1 occurrence);
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 28-May-2018