2018A&A...620A..94G


C.D.S. - SIMBAD4 rel 1.7 - 2021.03.01CET20:41:12

2018A&A...620A..94G - Astronomy and Astrophysics, volume 620A, 94-94 (2018/12-1)

Evolution of protoplanetary disks from their taxonomy in scattered light: spirals, rings, cavities, and shadows.

GARUFI A., BENISTY M., PINILLA P., TAZZARI M., DOMINIK C., GINSKI C., HENNING T., KRAL Q., LANGLOIS M., MENARD F., STOLKER T., SZULAGYI J., VILLENAVE M. and VAN DER PLAS G.

Abstract (from CDS):


Context. Dozens of protoplanetary disks have been imaged in scattered light during the last decade.
Aims. The variety of brightness, extension, and morphology from this census motivates a taxonomical study of protoplanetary disks in polarimetric light to constrain their evolution and establish the current framework of this type of observation.
Methods. We classified 58 disks with available polarimetric observations into six major categories (Ring, Spiral, Giant, Rim, Faint, and Small disks) based on their appearance in scattered light. We re-calculated the stellar and disk properties from the newly available Gaia DR2 and related these properties with the disk categories.
Results. More than half of our sample shows disk substructures. For the remaining sources, the absence of detected features is due to their faintness, their small size, or the disk geometry. Faint disks are typically found around young stars and typically host no cavity. There is a possible dichotomy in the near-infrared (NIR) excess of sources with spiral-disks (high) and ring-disks (low). Like spirals, shadows are associated with a high NIR excess. If we account for the pre-main sequence evolutionary timescale of stars with different mass, spiral arms are likely associated with old disks. We also found a loose, shallow declining trend for the disk dust mass with time.
Conclusions. Protoplanetary disks may form substructures like rings very early in their evolution but their detectability in scattered light is limited to relatively old sources (≥5Myr) where the recurrently detected disk cavities cause the outer disk to be illuminate. The shallow decrease of disk mass with time might be due to a selection effect, where disks observed thus far in scattered light are typically massive, bright transition disks with longer lifetimes than most disks. Our study points toward spirals and shadows being generated by planets of a fraction of a Jupiter mass to a few Jupiter masses in size that leave their (observed) imprint on both the inner disk near the star and the outer disk cavity.

Abstract Copyright: © ESO 2018

Journal keyword(s): planet-disk interactions - planets and satellites: formation - protoplanetary disks

Simbad objects: 76

goto Full paper

goto View the reference in ADS

Number of rows : 76

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 EM* LkHA 330 TT* 03 45 48.2804487421 +32 24 11.851014679   12.30 10.97     F7 125 0
2 V* RY Tau Or* 04 21 57.4132838427 +28 26 35.533990877 10.82 10.34 9.30 9.67 8.87 K1IV/Ve 661 1
3 V* UX Tau A TT* 04 30 03.9931880444 +18 13 49.476948664   12.92 11.15     K2Ve 333 0
4 V* HL Tau Or* 04 31 38.471952 +18 13 58.08504   15.89 14.49 14.39   K5 1240 0
5 V* GG Tau Or* 04 32 30.3318954228 +17 31 40.834888327 14.84 14.78 13.40 11.54   M0e+M2.0e 665 1
6 V* CI Tau Or* 04 33 52.0144455735 +22 50 30.093741884 14.97 15.09 13.80     K4IVe 285 1
7 EM* LkCa 15 Or* 04 39 17.7912813350 +22 21 03.387667491   13.01 12.03 11.61   K5:Ve 580 1
8 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 3642 0
9 V* GM Aur Or* 04 55 10.9813656049 +30 21 59.375978047 14.59 14.22 13.10     K3Ve 566 0
10 V* AB Aur Ae* 04 55 45.8459978418 +30 33 04.293281305 7.20 7.16 7.05 6.96 6.70 A0Ve 951 2
11 V* SU Aur Or* 04 55 59.3861369488 +30 34 01.499800471   10.33 9.30 9.17   G2IIIne 545 0
12 HD 31648 Ae* 04 58 46.2654165113 +29 50 36.990341242 7.84 7.78 7.62 7.76 7.43 A5Vep 411 0
13 V* V1366 Ori Ae* 05 16 00.4764811920 -09 48 35.394685295 10.19 10.16 9.84 9.77 9.63 B9.5V 168 0
14 HD 36112 Ae* 05 30 27.5286772598 +25 19 57.082162439   8.57 8.27     A8Ve 381 0
15 V* CQ Tau Ae* 05 35 58.4671238887 +24 44 54.086375712 11.290 10.780 10.000   8.33 F5IVe 265 0
16 NAME Ori I As* 05 38 -02.8           ~ 566 0
17 V* V1247 Ori dS* 05 38 05.2518310146 -01 15 21.696624736   10.18 9.82     F0V 80 0
18 NAME Ori A MoC 05 38 -07.1           ~ 2737 0
19 NAME GUM Nebula ISM 07 43 -42.1           ~ 393 1
20 V* AT Pyx Or* 08 28 40.6971304655 -33 46 22.287241515     12.7     K2.0 29 1
21 V* SY Cha Or* 10 56 30.3882538728 -77 11 39.402450501         11.29 K5Ve 115 0
22 V* SZ Cha Or* 10 58 16.7496916561 -77 17 17.183339177     12.68   10.62 K0e 106 0
23 V* TW Hya TT* 11 01 51.9054298616 -34 42 17.031550898   11.94 10.50 10.626 9.18 K6Ve 1596 1
24 V* CS Cha Or* 11 02 24.8849252208 -77 33 35.683462615   12.88 11.69   10.123 K2Ve 201 0
25 NAME Cha 1 MoC 11 06 48 -77 18.0           ~ 1009 1
26 V* DI Cha Or* 11 07 20.7272524388 -77 38 07.303742740   12.02 10.74 10.72   G2Ve 149 0
27 HD 97048 Ae* 11 08 03.3105687971 -77 39 17.491180130 9.03 8.76 9.00   8.64 A0Vep 467 0
28 V* VZ Cha Or* 11 09 23.7736314968 -76 23 20.855918834   13.82 12.94   12.14 K7e 128 0
29 V* CV Cha Or* 11 12 27.7052551478 -76 44 22.298597430   12.02 10.98 10.51 9.76 G9Ve 177 1
30 HD 100453 Ae* 11 33 05.5765928993 -54 19 28.543792679   8.09 7.79     A9Ve 216 1
31 HD 100546 Be* 11 33 25.4404858122 -70 11 41.239343121   6.71 6.30   6.64 A0VaekB8_lB 669 1
32 V* DZ Cha LM* 11 49 31.8520891363 -78 51 01.058647109     12.832   10.732 M0Ve 66 0
33 NAME Chamaeleon Region SFR 11 55 -78.0           ~ 708 0
34 V* T Cha Or* 11 57 13.5268556629 -79 21 31.521755129   10.00 11.86     K0e 241 1
35 NAME Lower Centaurus Crux As* 12 19 -57.1           ~ 372 1
36 CPD-68 1894 TT* 13 22 07.5420267499 -69 38 12.216304202   11.38 10.393   9.117 K1Ve 133 0
37 CD-40 8434 TT* 14 08 10.1545137760 -41 23 52.576649494   13.42 12.18 11.71 10.506 K7IVe 145 0
38 CPD-36 6759 Y*O 15 15 48.4459023859 -37 09 16.026315179   9.21 8.708     F8V 374 1
39 NAME Upper Centaurus Lupus As* 15 24 -41.9           ~ 378 1
40 HD 139614 Ae? 15 40 46.3818973118 -42 29 53.538928508   8.47 8.24     A9VekA5mA5(_lB) 167 0
41 V* GW Lup Or* 15 46 44.7292759994 -34 30 35.677245389   13.8       M1.5e 91 0
42 HD 141569 Y*O 15 49 57.7484743862 -03 55 16.344023102 7.22 7.20 7.12 7.00 7.04 A2VekB9mB9(_lB) 480 0
43 THA 15-12 Or* 15 56 09.2067120748 -37 56 06.126159332   13.12 11.93 11.45   M0e 276 0
44 HD 142666 TT* 15 56 40.0222941557 -22 01 40.004849949 9.41 9.37 8.82 8.31 8.01 F0V_sh 225 0
45 HD 142527 Ae* 15 56 41.8888096574 -42 19 23.245384377   9.04 8.34     F6III 503 1
46 V* RU Lup Or* 15 56 42.3109948086 -37 49 15.473469159 9.27 10.07 9.60     K7/M0e 399 0
47 HD 143006 Or* 15 58 36.9127773802 -22 57 15.221492622   10.92 10.14   8.70 G5IVe 176 0
48 V* RY Lup Or* 15 59 28.3852522995 -40 21 51.255321659   12.62 9.90     G8/K1IV-V 178 0
49 V* MY Lup TT* 16 00 44.5199369001 -41 55 30.931594414   12.64 12.17 11.06   K0 69 0
50 NAME Lup Cloud SFR 16 03 -38.1           ~ 549 0
51 HD 325367 Or* 16 03 05.4914377137 -40 18 25.426543472   11.40 8.50     M0 292 0
52 RX J1604.3-2130 * 16 04 21.66 -21 30 28.4       11.8   K2 26 0
53 HD 144432 Ae* 16 06 57.9530266912 -27 43 09.758016578 8.47 8.53 8.19 7.82 7.53 A9/F0V 218 1
54 THA 15-20 TT* 16 07 11.5876160594 -39 03 47.490881982   16.25 14.58 14.11 12.92 M0.5 79 0
55 IRAS 16051-3820 Y*O 16 08 30.6992185515 -38 28 26.847010777   11.89 11.15 10.67   K2 42 0
56 V* V856 Sco Ae* 16 08 34.2868591379 -39 06 18.326059778 7.66 7.41 7.05 6.92   A7IIIne_sh 359 0
57 THA 15-33 TT* 16 08 54.6847312618 -39 37 43.145460615   15.34 13.98 13.29   M1IVe 66 0
58 NAME Upper Sco Association As* 16 12 -23.4           ~ 1085 1
59 HD 145718 Ae* 16 13 11.5918477499 -22 29 06.620148459   9.29 8.86     A5Ve 88 0
60 NAME ASSOC II SCO As* 16 15 -24.2           ~ 1160 1
61 WRAY 15-1443 TT* 16 15 20.2339854383 -32 55 05.097043020 13.88 13.22 12.00 11.21 10.50 K5 70 0
62 GSS 39 Y*O 16 26 45.0321556934 -24 23 07.808781522           M0 150 1
63 Haro 1-8 Or* 16 26 47.4281589964 -23 14 52.213287086   14.1       ~ 48 0
64 EM* SR 21A TT* 16 27 10.2776332501 -24 19 12.620553212   16.08 14.10     G1 244 1
65 IRAS 16245-2423 TT* 16 27 37.1911764648 -24 30 35.031583716       16.66 14.67 B5-F2 243 0
66 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3133 1
67 Haro 1-16 Or* 16 31 33.4638378966 -24 27 37.158295501   14.02 12.80     K3e 187 0
68 HD 150193A Ae* 16 40 17.923 -23 53 45.17   9.39 8.88     ~ 6 0
69 HD 150193 Be* 16 40 17.9242900066 -23 53 45.192676418 9.69 9.32 8.79 8.41   B9.5Ve 296 0
70 EM* AS 209 Or* 16 49 15.3035547820 -14 22 08.642015783   12.62 11.28     K4Ve 255 0
71 V* AK Sco Ae* 16 54 44.8497760618 -36 53 18.560813962 9.80 9.63 9.00     F5V 244 1
72 HD 163296 Ae* 17 56 21.2882188601 -21 57 21.872343282 7.00 6.93 6.85 6.86 6.67 A1Vep 840 0
73 HD 319139 LM* 18 14 10.4818974563 -32 47 34.516106830   11.47 10.68   9.11 K5+K7 306 0
74 HD 169142 Ae* 18 24 29.7799676975 -29 46 49.328597698   8.42 8.16     F1VekA3mA3_lB? 352 2
75 2MASS J18521730-3700119 TT* 18 52 17.3009516263 -37 00 11.951133600   12.7 12.194   10.842 K7V 45 0
76 HD 179218 Ae* 19 11 11.2540715594 +15 47 15.632212730 7.55 7.476 7.39 7.25 7.21 A0Ve 225 0

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 2018A&A...620A..94G and select 'bookmark this link' or equivalent in the popup menu


2021.03.01-20:41:12

© Université de Strasbourg/CNRS

    • Contact