2020A&A...635A.105P


Query : 2020A&A...635A.105P

2020A&A...635A.105P - Astronomy and Astrophysics, volume 635A, 105-105 (2020/3-1)

Hints on the origins of particle traps in protoplanetary disks given by the Mdust - M relation.

PINILLA P., PASCUCCI I. and MARINO S.

Abstract (from CDS):


Context. Demographic surveys of protoplanetary disks, carried out mainly with the Atacama Large Millimeter/submillimete Array, have provided access to a large range of disk dust masses (Mdust) around stars with different stellar types and in different star-forming regions. These surveys found a power-law relation between Mdust and M* that steepens in time, but which is also flatter for transition disks (TDs).
Aims. We aim to study the effect of dust evolution in the Mdust-M* relation. In particular, we are interested in investigating the effect of particle traps on this relation.
Methods. We performed dust evolution models, which included perturbations to the gas surface density with different amplitudes to investigate the effect of particle trapping on the Mdust-M* relation. These perturbations were aimed at mimicking pressure bumps that originated from planets. We focused on the effect caused by different stellar and disk masses based on exoplanet statistics that demonstrate a dependence of planet mass on stellar mass and metallicity.
Results. Models of dust evolution can reproduce the observed Mdust-M* relation in different star-forming regions when strong pressure bumps are included and when the disk mass scales with stellar mass (case of Mdisk=0.05 M* in our models). This result arises from dust trapping and dust growth beyond centimeter-sized grains inside pressure bumps. However, the flatter relation of Mdust-M* for TDs and disks with substructures cannot be reproduced by the models unless the formation of boulders is inhibited inside pressure bumps.
Conclusions. In the context of pressure bumps originating from planets, our results agree with current exoplanet statistics on giant planet occurrence increasing with stellar mass, but we cannot draw a conclusion about the type of planets needed in the case of low-mass stars. This is attributed to the fact that for M*<1M, the observed Mdust obtained from models is very low due to the efficient growth of dust particles beyond centimeter-sizes inside pressure bumps.

Abstract Copyright: © P. Pinilla et al. 2020

Journal keyword(s): accretion, accretion disks - protoplanetary disks - planets and satellites: formation

Simbad objects: 78

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Number of rows : 78
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 [BCG93] 1 TT* 04 14 17.6095515480 +28 06 09.654704388 18.04         M4.5 87 0
2 V* V892 Tau Ae* 04 18 40.6157618376 +28 19 15.625058880   16.6 14.69 14.35   A0Ve 280 0
3 NAME Auriga reg 04 20 00.0 +38 05 00           ~ 187 0
4 V* RY Tau Or* 04 21 57.4092550080 +28 26 35.555316612 10.82 10.34 9.30 9.67 8.87 K1IV/Ve 673 1
5 V* FT Tau Or* 04 23 39.1888788312 +24 56 14.250818940   16.15 14.93 14.70   M2.8 127 0
6 V* IP Tau Or* 04 24 57.0824018640 +27 11 56.539953888   14.50   12.46   M0:Ve 208 0
7 V* IQ Tau Or* 04 29 51.5569574040 +26 06 44.859710736 15.43   13.80 12.28 11.11 M0.5 219 0
8 V* UX Tau A TT* 04 30 03.9932216088 +18 13 49.469925504   12.92 11.15     K2Ve 342 0
9 V* HL Tau Or* 04 31 38.5107609312 +18 13 57.859747968   15.89 14.49 14.39   K5 1328 0
10 V* UZ Tau Y*O 04 32 42.81 +25 52 31.3           M4Ve+M1/3Ve 299 0
11 V* DL Tau Or* 04 33 39.0767679288 +25 20 38.101382952 14.04 14.59 13.40 11.85 10.89 K7Ve 309 0
12 V* DM Tau Or* 04 33 48.7336763736 +18 10 09.973460280 14.30 14.82 14.00     M2Ve 582 0
13 V* CI Tau Or* 04 33 52.0143963264 +22 50 30.094090908 14.97 15.09 13.80     K4IVe 309 1
14 V* AA Tau Or* 04 34 55.4201902392 +24 28 53.033624580 13.14 13.34 12.20     K5Ve 682 0
15 V* DN Tau Or* 04 35 27.3776226144 +24 14 58.910343720 13.56 12.88 11.50 11.79   M1:Ve 368 0
16 EM* LkCa 15 Or* 04 39 17.7911622816 +22 21 03.390090984   13.01 12.03 11.61   K5:Ve 615 1
17 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 3955 0
18 V* GO Tau Or* 04 43 03.0761840904 +25 20 18.706850340   16.2 14.40     M2.3 177 0
19 V* DS Tau Or* 04 47 48.5954691000 +29 25 11.191621512 13.11 13.16 12.30 12.37 10.80 K4Ve 231 0
20 V* GM Aur Or* 04 55 10.9815576936 +30 21 59.373771876 14.59 13.351 12.242 11.798   K3Ve 617 0
21 HD 31648 Ae* 04 58 46.2655706952 +29 50 36.987625680 7.84 7.78 7.62 7.76 7.43 A5Vep 459 0
22 V* V1366 Ori Ae* 05 16 00.4765181328 -09 48 35.393784012 10.19 10.16 9.84 9.77 9.63 B9.5V 184 0
23 HD 36112 Ae* 05 30 27.5285630040 +25 19 57.076288752   8.57 8.27     A8Ve 419 0
24 V* CQ Tau Ae* 05 35 58.4666264136 +24 44 54.091450572 11.290 10.780 10.000   8.33 F5IVe 283 0
25 V* V1247 Ori dS* 05 38 05.2519466880 -01 15 21.698856468   10.18 9.82     F0V 93 0
26 NAME sigma Orionis Cluster MGr 05 38 42 -02 36.0           ~ 524 0
27 V* SY Cha Or* 10 56 30.3883129248 -77 11 39.401977596         11.29 K5Ve 118 0
28 V* SZ Cha Or* 10 58 16.7500775160 -77 17 17.185749900     12.68   10.62 K0e 112 0
29 V* TW Hya TT* 11 01 51.9053285064 -34 42 17.033218380   11.94 10.50 10.626 9.18 K6Ve 1745 1
30 NAME Cha 1 MoC 11 06 48 -77 18.0           ~ 1069 1
31 HD 97048 Ae* 11 08 03.3109731720 -77 39 17.490777444 9.03 8.76 9.00   8.64 A0Vep 497 0
32 HD 100546 Be* 11 33 25.4408872296 -70 11 41.241297948   6.71 6.30   6.64 A0VaekB8_lB 719 1
33 V* T Cha Or* 11 57 13.5245085552 -79 21 31.530508884   10.00 11.86     K0e 255 1
34 CPD-36 6759 Y*O 15 15 48.4460065200 -37 09 16.024369824   9.21 8.708     F8V 413 1
35 CD-33 10685 Or* 15 45 12.8678037432 -34 17 30.644403036 12.47 11.56 10.224 9.60 8.685 K3Ve 248 1
36 V* GW Lup Or* 15 46 44.7290527536 -34 30 35.677420056   13.8       M1.5e 107 0
37 THA 15-12 Or* 15 56 09.2066646912 -37 56 06.126118692   13.12 11.93 11.45   M0e 339 0
38 HD 142666 TT* 15 56 40.0221861696 -22 01 40.005872148 9.41 9.37 8.82 8.31 8.01 F0V_sh 239 0
39 V* RU Lup Or* 15 56 42.3108692112 -37 49 15.473946900 9.27 10.07 9.60     K7/M0e 425 0
40 WRAY 15-1400 TT* 15 59 16.4717314824 -41 57 10.300018176   13.5 12.0     K7IVe 78 0
41 V* RY Lup Or* 15 59 28.3864710696 -40 21 51.249496176   12.62 9.90     G8/K1IV-V 197 0
42 V* MY Lup TT* 16 00 44.5202267160 -41 55 30.935126748   12.64 12.17 11.06   K0 84 0
43 NAME Lupus Complex SFR 16 03 -38.1           ~ 613 0
44 ATO J241.0901-21.5080 Y*O 16 04 21.6547947840 -21 30 28.550063304   13.3       K2 109 0
45 HD 144006 * 16 05 02.3799607872 -38 24 39.806308548   10.47 9.75     F0/2 4 0
46 2MASS J16070854-3914075 LM* 16 07 08.5530917712 -39 14 07.494035352   17.85   18.67 17.86 M1.75 30 0
47 THA 15-20 TT* 16 07 11.5873449384 -39 03 47.492129340   16.25 14.58 14.11 12.92 M0.5 89 0
48 V* V1279 Sco Or* 16 08 22.4935277520 -39 04 46.427612052   14.99 13.66 11.70 11.21 M0.4 101 1
49 THA 15-26 Y*O 16 08 25.7633674272 -39 06 01.247043888   16.62 15.43 14.97 13.12 M5 57 0
50 IRAS 16051-3820 Y*O 16 08 30.6994064064 -38 28 26.846324004   11.89 11.15 10.67   K2 53 0
51 V* V1094 Sco TT* 16 08 36.1772010696 -39 23 02.464980972 16.01 15.00 13.48 12.47 11.45 ~ 63 1
52 THA 15-33 TT* 16 08 54.6849382512 -39 37 43.145069664   15.34 13.98 13.29   M1IVe 73 0
53 THA 15-35 Or* 16 09 01.8486544824 -39 05 12.414717240   15.33 14.12 14.35 12.54 M5.5 89 0
54 Sz 118 Y*O 16 09 48.6562295568 -39 11 16.847425032   18.32 16.90 16.61 15.00 K6 53 0
55 THA 15-42 Y*O 16 10 51.5849835192 -38 53 13.767885384   15.89 14.48 14.44 12.95 M1e 61 0
56 V* V866 Sco Or* 16 11 31.345632 -18 38 25.96200   13.98 12.63 12.81   K0e+K5e 262 0
57 NAME Upper Sco Association As* 16 12 -23.4           ~ 1201 1
58 WRAY 15-1443 TT* 16 15 20.2341630672 -32 55 05.097631872 13.88 13.22 12.00 11.21 10.50 K5 77 0
59 2MASS J16230923-2417047 Y*O 16 23 09.2283172152 -24 17 05.013918240   14.3 12.75     M 33 0
60 BKLT J162538-242238 Y*O 16 25 38.1274773528 -24 22 36.185318004           M0 29 0
61 EM* SR 4 Or* 16 25 56.1659023848 -24 20 48.240627072     12.80 11.7 10.7 K0:Ve 168 1
62 Elia 2-20 TT* 16 26 18.8775818016 -24 28 19.695035064           ~ 106 1
63 DoAr 25 TT* 16 26 23.6911292736 -24 43 13.888543800       12.65   K5 145 0
64 Elia 2-24 TT* 16 26 24.0886188024 -24 16 13.448569260   16.3 14.40 15.81 13.97 K6 141 1
65 [GY92] 91 Y*O 16 26 40.46952 -24 27 14.4720           ~ 69 1
66 GSS 39 Y*O 16 26 45.0318401664 -24 23 07.793180124           M0 170 1
67 EM* SR 24A TT* 16 26 58.5134422944 -24 45 36.722580480       14.15 12.87 K1 96 0
68 EM* SR 21A TT* 16 27 10.2778380120 -24 19 12.622467720   16.08 14.10     G1 256 1
69 DoAr 33 TT* 16 27 39.0123517344 -23 58 18.709495500   15.7   13.24 12.02 K4 55 0
70 ROX 27 TT* 16 27 39.4295731464 -24 39 15.527230272       15.76 14.03 M0+M4 102 0
71 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3361 1
72 Haro 1-16 Or* 16 31 33.4634997336 -24 27 37.158728076   14.02 12.80     K3e 205 0
73 2MASS J16335560-2442049 Y*O 16 33 55.6148566800 -24 42 05.002391016           K7 46 0
74 2MASS J16394544-2402039 TT* 16 39 45.4432704120 -24 02 03.885092160   16.0 12.7     K 27 0
75 EM* AS 209 Or* 16 49 15.3034917000 -14 22 08.643317664   12.62 11.28     K4Ve 307 0
76 HD 163296 Ae* 17 56 21.2881851168 -21 57 21.871819008 7.00 6.93 6.85 6.86 6.67 A1Vep 959 0
77 HD 319139 SB* 18 14 10.4818675368 -32 47 34.516836060   11.47 10.68   9.11 K5+K7 329 0
78 HD 169142 Ae* 18 24 29.7799891464 -29 46 49.327400568   8.42 8.16     F1VekA3mA3_lB? 388 2

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2022.07.06-09:00:06

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