2011A&A...527A.119B


C.D.S. - SIMBAD4 rel 1.7 - 2020.09.22CEST08:02:17

2011A&A...527A.119B - Astronomy and Astrophysics, volume 527A, 119-119 (2011/3-1)

Single peaked CO emission line profiles from the inner regions of protoplanetary disks.

BAST J.E., BROWN J.M., HERCZEG G.J., VAN DISHOECK E.F. and PONTOPPIDAN K.M.

Abstract (from CDS):

Protoplanetary disks generally exhibit strong line emission from the CO fundamental v=1-0 ro-vibrational band around 4.7µm. The lines are usually interpreted as being formed in the Keplerian disk, as opposed to other kinematic components of the young stellar system. This paper investigates a set of disks that show CO emission line profiles characterized by a single, narrow peak and a broad base extending to >50km/s, not readily explained by just Keplerian motions of gas in the inner disk. High resolution (R=105) M-band spectroscopy has been obtained using CRIRES at the Very Large Telescope in order to fully resolve fundamental ro-vibrational CO emission line profiles around 4.7µm. Line profiles with a narrow peak and broad wings are found for 8 disks among a sample of ∼50 disks around T Tauri stars with CO emission. The lines are very symmetric, have high line/continuum ratios and have central velocity shifts of <5km/s relative to the stellar radial velocity. The disks in this subsample are accreting onto their central stars at high rates relative to the parent sample. All 8 disks show CO emission lines from the v=2 vibrational state and 4/8 disks show emission up to v=4. Excitation analyses of the integrated line fluxes reveal a significant difference between typical rotational (∼300-800K) and vibrational (∼1700K) temperatures, suggesting that the lines are excited, at least in part, by UV-fluorescence. For at least one source, the narrow and broad components show different excitation temperatures, but generally the two component fits have similar central velocities and temperature. Analysis of their spatial distribution shows that the lines are formed within a few AU of the central star. It is concluded that these broad centrally peaked line profiles are inconsistent with the double peaked profiles expected from just an inclined disk in Keplerian rotation. Models in which the low velocity emission arises from large disk radii are excluded based on the small spatial distribution. Alternative non-Keplerian line formation mechanisms are discussed, including thermally and magnetically launched winds and funnel flows. The most likely interpretation is that the broad-based centrally peaked line profiles originate from a combination of emission from the inner part (<a few AU) of a circumstellar disk, perhaps with enhanced turbulence, and a slow moving disk wind, launched by either EUV emission or soft X-rays.

Abstract Copyright:

Journal keyword(s): protoplanetary disks - line: profiles - stars: low-mass - planets and satellites: formation - accretion, accretion disks

CDS comments: Table 3 : sources IRS 48 and 51 not identified.

Simbad objects: 44

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Number of rows : 44

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 * 41 Ari ** 02 49 59.0332406 +27 15 37.826018   3.498 3.594     B8Vn 149 0
2 EM* LkHA 330 TT* 03 45 48.2804487421 +32 24 11.851014679   12.30 10.97     F7 121 0
3 V* FN Tau Or* 04 14 14.5943659839 +28 27 58.063377983     14.70 13.68   M5 141 0
4 V* CW Tau Or* 04 14 17.0041128798 +28 10 57.765657757 13.92 13.64 12.36 12.86   K0Ve 315 0
5 V* DF Tau Or* 04 27 02.7917481241 +25 42 22.456361256 11.97 12.25 11.42 10.31 9.14 M3Ve 460 1
6 V* AA Tau Or* 04 34 55.4222683130 +24 28 53.038273587 13.14 13.34 12.20     K5Ve 630 0
7 V* DR Tau Or* 04 47 06.2152696011 +16 58 42.814250257 12.03 11.86 10.50 12.19   K5Ve 469 0
8 V* AB Aur Ae* 04 55 45.8459978418 +30 33 04.293281305 7.20 7.16 7.05 6.96 6.70 A0Ve 934 2
9 * bet Tau PM* 05 26 17.51312 +28 36 26.8262 1.03 1.52 1.65 1.66 1.76 B7III 347 1
10 V* GW Ori Or* 05 29 08.3925564419 +11 52 12.653756566   10.83 10.10 9.52   G5/8Ve 299 0
11 * chi Car bC* 07 56 46.7232212143 -52 58 56.394323256 2.64 3.267 3.431     B3IV 136 1
12 V* TW Hya TT* 11 01 51.9054298616 -34 42 17.031550898   11.94 10.50 10.626 9.18 K6Ve 1545 1
13 V* VW Cha Or* 11 08 01.3974165580 -77 42 28.579297348 13.91 14.04 12.80   10.69 K7+M0 167 0
14 V* VZ Cha Or* 11 09 23.7736314968 -76 23 20.855918834   13.82 12.94   12.14 K7e 124 0
15 V* CV Cha Or* 11 12 27.7052551478 -76 44 22.298597430   12.02 10.98 10.51 9.76 G9Ve 171 1
16 * lam Cen * 11 35 46.8790838328 -63 01 11.396483522 2.96 3.10 3.14 3.10 3.11 B9III 122 0
17 * del Crv PM* 12 29 51.8551642 -16 30 55.552542 2.80 2.89 2.94 2.99 3.03 A0IV(n)kB9 185 0
18 * bet Lup PM* 14 58 31.92536 -43 08 02.2699 1.59 2.46 2.68 2.78 2.95 B2III 177 0
19 CPD-36 6759 Y*O 15 15 48.4459023859 -37 09 16.026315179   9.21 8.708     F8V 358 1
20 * tau Lib SB* 15 38 39.3694957 -29 46 39.895604   3.481 3.642     B2.5V 145 0
21 CD-35 10525 Or* 15 49 12.1055573607 -35 39 05.053991067 12.19 12.76 11.66 11.15   K7Ve 238 0
22 HD 141569 pr* 15 49 57.7484743862 -03 55 16.344023102 7.22 7.20 7.12 7.00 7.04 A2VekB9mB9(_lB) 473 0
23 * chi Lup SB* 15 50 57.5382881 -33 37 37.795321 3.77 3.909 3.946     B9III 289 0
24 HD 142527 Ae* 15 56 41.8888096574 -42 19 23.245384377   9.04 8.34     F6III 472 1
25 V* RU Lup Or* 15 56 42.3109948086 -37 49 15.473469159 9.27 10.07 9.60     K7/M0e 384 0
26 V* RY Lup Or* 15 59 28.3852522995 -40 21 51.255321659   12.62 9.90     G8/K1IV-V 168 0
27 HD 325367 Or* 16 03 05.4914377137 -40 18 25.426543472   11.40 8.50     M0 279 0
28 * bet01 Sco SB* 16 05 26.2319826 -19 48 19.630018 1.68 2.55 2.62 2.60 2.69 B1V 533 0
29 V* V866 Sco Or* 16 11 31.345632 -18 38 25.96200   13.98 12.63 12.81   K0e+K5e 247 0
30 * sig Sco bC* 16 21 11.3157134 -25 35 34.051476 2.32 3.02 2.89 1.69 1.58 O9.5(V)+B7(V) 827 0
31 Haro 1-4 Or* 16 25 10.508136 -23 19 14.78820       13.15   K4e 70 0
32 Elia 2-20 TT* 16 26 18.8782824640 -24 28 19.698059817           ~ 93 1
33 GSS 31 TT* 16 26 23.3694945462 -24 20 59.580653864   15.9 14.70 14.33 11.53 K0e 133 1
34 EM* SR 21A TT* 16 27 10.2776332501 -24 19 12.620553212   16.08 14.10     G1 233 1
35 EM* SR 9 Or* 16 27 40.2858402419 -24 22 04.132012501   12.91 11.533 11.11 10.00 K5e 249 0
36 Haro 1-16 Or* 16 31 33.4638378966 -24 27 37.158295501   14.02 12.80     K3e 176 0
37 V* V1003 Oph Or* 16 34 09.1694383329 -15 48 16.776308800           G5 87 0
38 V* VV Ser Ae* 18 28 47.8619658319 +00 08 39.924642619 12.99 12.63 11.80 11.01 10.24 A5Ve 228 0
39 V* S CrA Or* 19 01 08.597088 -36 57 19.89504   11.76 10.91 11.41   G0Ve+K0Ve 258 0
40 V* VV CrA Or* 19 03 06.7419790029 -37 12 49.683383133   16.45 14.67 14.12 11.62 K7 107 0
41 * zet Aql PM* 19 05 24.6080155 +13 51 48.518212 2.99 3.00 2.99 2.98 2.98 A0IV-Vnn 322 0
42 * lam Aql PM* 19 06 14.9397099975 -04 52 57.231496924 3.07 3.34 3.43 3.46 3.55 B8.5V 207 0
43 * chi01 Sgr ** 19 25 16.4901283 -24 30 30.859921   5.238 5.009 6.67   A3/5IV/V 67 0
44 * eta Ind dS* 20 44 02.3340423 -51 55 15.496981   4.767 4.495     A9IV 75 0

    Equat.    Gal    SGal    Ecl

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2020.09.22-08:02:17

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