2019A&A...632A..32M


C.D.S. - SIMBAD4 rel 1.7 - 2020.10.25CET09:13:35

2019A&A...632A..32M - Astronomy and Astrophysics, volume 632A, 32-32 (2019/12-0)

Carbon depletion observed inside T Tauri inner rims. Formation of icy, kilometer size planetesimals by 1 Myr.

McCLURE M.K.

Abstract (from CDS):


Context. The carbon content of protoplanetary disks is an important parameter to characterize planets formed at different disk radii. There is some evidence from far-infrared and submillimeter observations that gas in the outer disk is depleted in carbon, with a corresponding enhancement of carbon-rich ices at the disk midplane. Observations of the carbon content inside of the inner sublimation rim could confirm how much carbon remains locked in kilometer size bodies in the disk.
Aims. I aim to determine the density, temperature, and carbon abundance inside the disk dust sublimation rim in a set of T Tauri stars with full protoplanetary disks.
Methods. Using medium-resolution, near-infrared (0.8-2.5µm) spectra and the new Gaia DR2 distances, I self-consistently determine the stellar, extinction, veiling, and accretion properties of the 26 stars in my sample. From these values, and non-accreting T Tauri spectral templates, I extract the inner disk excess of the target stars from their observed spectra. Then I identify a series of C0 recombination lines in 18 of these disks and use the CHIANTI atomic line database with an optically thin slab model to constrain the average ne, Te, and nc for these lines in the five disks with a complete set of lines. By comparing these values with other slab models of the inner disk using the Cloudy photoionization code, I also constrain nH and the carbon abundance, XC, and hence the amount of carbon "missing" from the slab. For one disk, DR Tau, I use relative abundances for the accretion stream from the literature to also determine XSi and XN.
Results. The inner disks modeled here are extremely dense (nH∼1016cm–3), warm (Te∼4500K), and moderately ionized (logXe∼3.3). Three of the five modeled disks show robust carbon depletion up to a factor of 42 relative to the solar value. I discuss multiple ways in which the "missing" carbon could be locked out of the accreting gas. Given the high-density inner disk gas, evidence for radial drift, and lack of obvious gaps in these three systems, their carbon depletion is most consistent with the "missing" carbon being sequestered in kilometer size bodies. For DR Tau, nitrogen and silicon are also depleted by factors of 45 and 4, respectively, suggesting that the kilometer size bodies into which the grains are locked were formed beyond the N2 snowline. I explore briefly what improvements in the models and observations are needed to better address this topic in the future.

Abstract Copyright: © ESO 2019

Journal keyword(s): astrochemistry - line: formation - solid state: volatile - techniques: spectroscopic - protoplanetary disks - stars: variables: T Tauri, Herbig Ae/Be

VizieR on-line data: <Available at CDS (J/A+A/632/A32): table1.dat table2.dat list.dat sp/*>

Simbad objects: 31

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Number of rows : 31

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 V* CW Tau Or* 04 14 17.0041128798 +28 10 57.765657757 13.92 13.64 12.36 12.86   K0Ve 318 0
2 V* CX Tau Or* 04 14 47.8612023028 +26 48 11.013547235 16.48 15.93 14.50     M1.5Ve 152 0
3 IRAS 04125+2902 TT* 04 15 42.7868524357 +29 09 59.826220836 19.191 17.442 15.487 13.954 12.418 M0 33 0
4 V* FQ Tau Or* 04 19 12.812616 +28 29 32.98128       15.00   M3 98 0
5 V* BP Tau Or* 04 19 15.8342975037 +29 06 26.929456808   13.13 12.12 11.89   K5/7Ve 604 0
6 V* DE Tau Or* 04 21 55.6346296353 +27 55 06.184221341 15.18 15.13 13.80     M3Ve 224 0
7 V* RY Tau Or* 04 21 57.4132838427 +28 26 35.533990877 10.82 10.34 9.30 9.67 8.87 K1IV/Ve 653 1
8 V* FS Tau Or* 04 22 02.1925017485 +26 57 30.331063489 17.57   14.10 15.63   M3.5e+M0e 261 0
9 V* FT Tau Or* 04 23 39.1894939930 +24 56 14.248383831   16.15 14.93 14.70   M2.8 112 0
10 V* IQ Tau Or* 04 29 51.5569553814 +26 06 44.854858369 15.43   13.80 12.28 11.11 M0.5 200 0
11 NAME Tau-Aur Complex SFR 04 30 +25.0           ~ 1227 0
12 V* FX Tau Or* 04 30 29.618064 +24 26 45.02724   15.18 13.61 13.21   M4 143 0
13 V* DK Tau Or* 04 30 44.243376 +26 01 24.65328 13.32 14.59 13.05 12.08   K7e+K7e 298 0
14 V* FZ Tau Or* 04 32 31.7629319321 +24 20 03.057541003 16.15     15.04   M0 119 0
15 IRAS 04303+2240 Y*O 04 33 19.0746339919 +22 46 34.185095127           M0.5 65 0
16 V* GI Tau Or* 04 33 34.0608378045 +24 21 17.067391746 14.34   13.70 12.15 11.06 K5Ve 253 1
17 V* GK Tau Or* 04 33 34.5626781676 +24 21 05.854541262 15.50   13.00 12.02 10.62 K7:Ve 274 0
18 V* DL Tau Or* 04 33 39.0766866461 +25 20 38.097973550 14.04 14.59 13.40 11.85 10.89 K7Ve 286 0
19 V* DM Tau Or* 04 33 48.7335659850 +18 10 09.974471722 14.30 14.82 14.00     M2Ve 518 0
20 V* CI Tau Or* 04 33 52.0144455735 +22 50 30.093741884 14.97 15.09 13.80     K4IVe 270 1
21 V* HQ Tau Or* 04 35 47.3327991214 +22 50 21.639107658 15.01 14.15 12.02 11.18   K0 76 0
22 V* HP Tau Or* 04 35 52.7821592361 +22 54 23.158368128 17.39 14.9 14.90     K2-5e 190 0
23 CoKu HP Tau G3 TT* 04 35 53.4991854163 +22 54 09.000431829 18.21   14.8     M0.6 58 0
24 Haro 6-28 Or* 04 35 56.8652987075 +22 54 35.826437972 18.94         M3.1 85 0
25 V* DO Tau Or* 04 38 28.5882167490 +26 10 49.472067634 12.78 13.44 12.30 13.01   M1Ve 319 1
26 V* GN Tau Or* 04 39 20.922216 +25 45 02.02608 17.22     13.85   M2.5 85 0
27 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 3544 0
28 V* DR Tau Or* 04 47 06.2152696011 +16 58 42.814250257 12.03 11.86 10.50 12.19   K5Ve 472 0
29 V* DS Tau Or* 04 47 48.5954846337 +29 25 11.189809829 13.11 13.16 12.30 12.37 10.80 K4Ve 211 0
30 V* GM Aur Or* 04 55 10.9813656049 +30 21 59.375978047 14.59 14.22 13.10     K3Ve 556 0
31 V* TW Hya TT* 11 01 51.9054298616 -34 42 17.031550898   11.94 10.50 10.626 9.18 K6Ve 1555 1

    Equat.    Gal    SGal    Ecl

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2020.10.25-09:13:35

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