2010A&A...523A..69R


Query : 2010A&A...523A..69R

2010A&A...523A..69R - Astronomy and Astrophysics, volume 523, A69-69 (2010/11-2)

Detectability of giant planets in protoplanetary disks by CO emission lines.

REGALY Z., SANDOR Z., DULLEMOND C.P. and VAN BOEKEL R.

Abstract (from CDS):

Planets are thought to form in protoplanetary accretion disks around young stars. Detecting a giant planet still embedded in a protoplanetary disk would be very important and give observational constraints on the planet-formation process. However, detecting these planets with the radial velocity technique is problematic owing to the strong stellar activity of these young objects. We intend to provide an indirect method to detect Jovian planets by studying near infrared emission spectra originating in the protoplanetary disks around TTauri stars. Our idea is to investigate whether a massive planet could induce any observable effect on the spectral lines emerging in the disks atmosphere. As a tracer molecule we propose CO, which is excited in the ro-vibrational fundamental band in the disk atmosphere to a distance of ∼2-3AU (depending on the stellar mass) where terrestrial planets are thought to form. We developed a semi-analytical model to calculate synthetic molecular spectral line profiles in a protoplanetary disk using a double layer disk model heated on the outside by irradiation by the central star and in the midplane by viscous dissipation due to accretion. 2D gas dynamics were incorporated in the calculation of synthetic spectral lines. The motions of gas parcels were calculated by the publicly available hydrodynamical code FARGO which was developed to study planet-disk interactions. We demonstrate that a massive planet embedded in a protoplanetary disk strongly influences the originally circular Keplerian gas dynamics. The perturbed motion of the gas can be detected by comparing the CO line profiles in emission, which emerge from planet-bearing to those of planet-free disk models. The planet signal has two major characteristics: a permanent line profile asymmetry, and short timescale variability correlated with the orbital phase of the giant planet. We have found that the strength of the asymmetry depends on the physical parameters of the star-planet-disk system, such as the disk inclination angle, the planetary and stellar masses, the orbital distance, and the size of the disk inner cavity. The permanent line profile asymmetry is caused by a disk in an eccentric state in the gap opened by the giant planet. However, the variable component is a consequence of the local dynamical perturbation by the orbiting giant planet. We show that a forming giant planet, still embedded in the protoplanetary disk, can be detected using contemporary or future high-resolution near-IR spectrographs like VLT/CRIRES and ELT/METIS.

Abstract Copyright:

Journal keyword(s): accretion, accretion disks - line: profiles - stars: variables: T Tauri, Herbig Ae/Be - planetary systems - methods: numerical - techniques: spectroscopic

Simbad objects: 27

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Number of rows : 27
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 IC 348 OpC 03 44 31.7 +32 09 32           ~ 1368 1
2 V* HL Tau Or* 04 31 38.5107609312 +18 13 57.859747968   15.89 14.49 14.39   K5 1393 0
3 IRAS 04287+1807 mul 04 31 38.8 +18 13 57           ~ 796 0
4 V* AA Tau Or* 04 34 55.4201902392 +24 28 53.033624580 13.14 13.34 12.20 12.03   K5Ve 714 0
5 V* DR Tau Or* 04 47 06.2151561264 +16 58 42.813872580 12.03 11.86 10.50 12.19   K5Ve 526 0
6 V* V836 Tau TT* 05 03 06.5988375912 +25 23 19.606639488   15.00 13.49 13.48   K7/M0Ve 232 0
7 NAME Ori Trapezium OpC 05 35 16.5 -05 23 14           ~ 1598 1
8 M 36 OpC 05 36 20.2 +34 08 06   6.09 6.0     ~ 182 2
9 LDN 1641 MoC 05 39.0 -07 00           ~ 475 0
10 NGC 2024 Cl* 05 41 43 -01 50.5           ~ 1140 1
11 NAME LDN 1630N Cl* 05 46 47.0 +00 09 50           ~ 13 1
12 * bet Pic PM* 05 47 17.0876901 -51 03 59.441135 4.13 4.03 3.86 3.74 3.58 A6V 1860 1
13 NAME Orion Molecular Cloud MoC 05 56 -01.8           ~ 1065 1
14 HD 44627 Er* 06 19 12.9130449912 -58 03 15.527294208   10.01 9.205   8.185 K1V(e) 169 1
15 NGC 2264 OpC 06 40 52.1 +09 52 37           ~ 1761 0
16 NGC 2362 OpC 07 18 41.0 -24 57 14           ~ 403 0
17 NAME TW Hya b Pl? 11 01 51.9054298616 -34 42 17.031550898           ~ 9 1
18 V* CT Cha Or* 11 04 09.0989256840 -76 27 19.329779664   13.44 13.00   10.89 K7Ve 128 0
19 TWA 27 LM* 12 07 33.4675524840 -39 32 54.016625184     19.95 17.99 15.88 M8IVe 332 0
20 CPD-36 6759 Y*O 15 15 48.4460065200 -37 09 16.024369824   9.21 8.708     F8V 445 1
21 V* GQ Lup Or* 15 49 12.1053805848 -35 39 05.058139788 12.19 12.76 11.66 11.15   K7Ve 283 1
22 UScoCTIO 108 LM* 16 05 54.0734809368 -18 18 44.376318180           M7 42 0
23 V* V866 Sco Or* 16 11 31.345632 -18 38 25.96200   13.98 12.63 12.81   K0e+K5e 277 0
24 EM* SR 21A TT* 16 27 10.2778380120 -24 19 12.622467720   16.08 14.10     G1 267 1
25 SCR J1845-6357 LM* 18 45 05.2532493080 -63 57 47.450109578     17.40 14.99 12.46 M8.5V 69 1
26 * alf PsA PM* 22 57 39.04625 -29 37 20.0533 1.31 1.25 1.16 1.11 1.09 A4V 1216 3
27 HD 218396 El* 23 07 28.7157209544 +21 08 03.310767492   6.21 5.953     F0+VkA5mA5 1101 0

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2023.09.29-15:29:12

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