2023A&A...671A.140G


Query : 2023A&A...671A.140G

2023A&A...671A.140G - Astronomy and Astrophysics, volume 671A, 140 (2023/3-1)

Relation between metallicities and spectral energy distributions of Herbig Ae/Be stars A potential link with planet formation.

GUZMAN-DIAZ J., MONTESINOS B., MENDIGUTIA I., KAMA M., MEEUS G., VIOQUE M., OUDMAIJER R.D. and VILLAVER E.

Abstract (from CDS):

Context. Most studies devoted to Herbig Ae/Be stars (HAeBes) assume solar metallicity. However, the stellar metallicity, [M/H], is a fundamental parameter that can strongly differ depending on the source and may have important implications for planet formation. It has been proposed that the deficit of refractory elements observed in the surfaces of some HAeBes may be linked to the presence of cavities in their disks and is likely caused by Jovian planets that trap the metal-rich content.
Aims. This work aims to provide a robust test on the previous proposal by analyzing the largest sample of HAeBes characterized by homogeneously derived [M/H] values and stellar and circumstellar properties.
Methods. The spectra of 67 HAeBes, along with their well-known properties drawn from our previous work, have been collected from the ESO Science Archive Facility. Their [M/H] values were derived based on the comparison with Kurucz synthetic models. Statistical analyses were carried out with the aim to test the potential relation between [M/H] and the Meeus group I sources, with spectral energy distributions (SEDs) associated with the presence of cavities potentially carved by giant planets. We critically analyzed the eventual link between [M/H], the SED groups, and the presence of such planets.
Results. Our statistical study robustly confirms that group I sources tend to have a lower [M/H] (typically ∼ -0.10) than that of group II HAeBes (∼ +0.14). A similar analysis involving SED-based transitional disks, with infrared excess only at wavelengths of ≥2.2 µm, does not reveal such a relation with [M/H]. This result indicates that not all processes capable of creating holes in the inner dust disks end up having an effect on the stellar abundances. The spatial distributions of group I and II sources are similar, at least within the available range of distances to the galactic centre and the galactic plane, for which the observed [M/H] differences are not driven by environmental effects. In addition, group I sources tend to have stronger (sub-) mm continuum emission presumably related to the presence of giant planets. Indeed, literature results indicate that disk substructures probably associated with the presence of giant planets are up to ten times more frequent in group I HAeBes than in group II. Finally, along with the metallicities derived for the whole sample, surface gravities and projected rotational velocities are additional outcomes reported in this work.
Conclusions. We provide indirect evidence to suggest that giant planets are more frequent around group I/low [M/H] stars than around the rest of the HAeBes. However, a direct test of the previous hypothesis requires multiple detections of forming planets in their disks. Such detections have so far been limited to the candidate around the metal depleted ([M/H] = -0.35 ± -0.25) group I HAeBe star AB Aur, which is consistent with our findings.

Abstract Copyright: © The Authors 2023

Journal keyword(s): protoplanetary disks - planet-disk interactions - stars: pre-main sequence - stars: variables: T Tauri, Herbig Ae/Be - stars: fundamental parameters

Simbad objects: 72

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Number of rows : 72
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024
#notes
1 CD-53 251 Ae? 01 17 43.4985952032 -52 33 30.791840040   11.28 10.75     F3Ve 31 0
2 * 49 Cet PM* 01 34 37.7786780856 -15 40 34.898673000   5.667 5.607   5.54 A1V 303 0
3 V* AB Aur Ae* 04 55 45.8458932216 +30 33 04.292077032 7.20 7.16 7.05 6.96 6.70 A0Ve 1068 2
4 HD 31648 Ae* 04 58 46.2655706952 +29 50 36.987625680 7.84 7.78 7.62 7.76 7.43 A5Vep 521 0
5 V* UX Ori Ae* 05 04 29.9878898040 -03 47 14.286732072 10.25 10.93 8.70 9.62 9.43 A4IVe 363 1
6 V* V1366 Ori Ae* 05 16 00.4765181328 -09 48 35.393784012 10.19 10.16 9.84 9.77 9.63 B9.5V 209 0
7 HD 290380 EB* 05 23 31.0101754824 -01 04 23.701574136   10.97 10.41 10.25 9.79 keF6IVeb 41 0
8 HD 287823 Y*O 05 24 08.0485208544 +02 27 46.884084984   9.91 9.74     A0 52 0
9 HD 287841 Y*O 05 24 42.8032369656 +01 43 48.249234516 10.55 10.45 10.17 9.99 9.80 A8V 110 0
10 V* CO Ori Or* 05 27 38.3386648 +11 25 38.974625 12.96 12.33 10.30 10.33 9.63 F7Ve 168 0
11 HD 35929 dS* 05 27 42.7906489200 -08 19 38.446702140   8.55 8.11     F2IV/V 111 0
12 HD 290500 Ae? 05 29 48.0515601936 -00 23 43.508069160   11.35 11.04     A2 33 0
13 HD 244314 Or* 05 30 19.0247390376 +11 20 20.002720452   10.33 10.18     A1V 28 0
14 HD 36112 Ae* 05 30 27.5285630040 +25 19 57.076288752   8.57 8.27     A8Ve 469 0
15 HD 244604 Or* 05 31 57.2511172320 +11 17 41.368840404   9.61 9.43     A0Vesh 75 0
16 V* RY Ori Or* 05 32 09.9419233368 -02 49 46.770599784 12.62 12.76 10.80 10.82 10.34 F7 62 0
17 HD 36917 Or* 05 34 46.9822530528 -05 34 14.583314568   8.13 8.03     B9III/IV 153 0
18 HD 245185 Ae* 05 35 09.6034684104 +10 01 51.465413208 10.05 10.07 9.93     A0Vae 127 0
19 V* NV Ori Ae* 05 35 31.3686116448 -05 33 08.872027056 10.36 10.21 8.70 9.48 9.22 F6IIIe 105 0
20 V* T Ori Ae* 05 35 50.4482802768 -05 28 34.925254536 12.724 11.637 11.248 10.09 10.043 A8VnekA1mA2_lB 247 0
21 V* CQ Tau Ae* 05 35 58.4666264136 +24 44 54.091450572 11.290 10.780 10.000   8.33 F5IVe 310 0
22 HD 37258 Ae* 05 36 59.2496063912 -06 09 16.331028249   9.72 9.61 9.56   A3V_sh 135 0
23 HD 290770 Em* 05 37 02.4474064872 -01 37 21.363674700   9.29 9.30     B9 43 0
24 V* BF Ori Ae* 05 37 13.2623828280 -06 35 00.568242528 10.37 10.00 9.69 10.06 9.31 A7III 293 0
25 HD 37357 Ae* 05 37 47.0794735560 -06 42 30.209473224   8.96 8.85     A3VankA1 109 0
26 V* V1247 Ori dS* 05 38 05.2519466880 -01 15 21.698856468   10.18 9.82     F0V 115 0
27 V* V599 Ori Or* 05 38 58.6396084320 -07 16 45.626538792   15.39 13.70 12.61   A8.9 58 0
28 V* V350 Ori LP* 05 40 11.7638894112 -09 42 11.086012692 12.74 12.08 11.42 11.38 10.96 A7V 77 0
29 HD 38120 Be* 05 43 11.8932782280 -04 59 49.889995692 9.08 9.10 9.1     B9Vnne 90 0
30 * del Dor * 05 44 46.3699967519 -65 44 07.793159129 4.69 4.57 4.36 4.10 3.93 A7V 128 0
31 2MASS J06065848-0555066 TT* 06 06 58.4991960744 -05 55 06.700428156   12.97 12.44     A0 19 0
32 EM* LkHA 339 Ae* 06 10 57.8449670232 -06 14 39.659250840   14.44 13.60 13.44 12.50 A1e 36 0
33 NGC 2264 84 TT* 06 40 42.1820308368 +09 33 37.422060732 12.575 12.57 12.01 11.74 11.33 G0 77 0
34 NGC 2264 108 TT* 06 40 51.1854488784 +09 44 46.109300100 12.684 12.42 12.004 11.661 11.35 F8V 78 0
35 2MASS J06495854-0738522 TT* 06 49 58.5543923232 -07 38 52.253360268   14.06 13.40     B9 20 0
36 HD 68695 Y*O 08 11 44.5714665288 -44 05 08.777141772   9.93 9.87     A3VbekA0mA0_lB 43 0
37 IRAS F08432-5945 Ae? 08 44 23.6523525384 -59 56 57.876645408   10.96 10.91     A5V 13 0
38 IRAS 08469-4037 Ae? 08 48 45.6634197192 -40 48 21.082180356   12.63 12.34     A0 14 0
39 TYC 8593-2802-1 * 09 42 40.3389047976 -56 15 34.099594920   12.17 11.82     A7? 13 1
40 HD 87048 * 10 02 42.8448454104 +03 40 12.496076256   9.25 8.78     A6V 13 0
41 HD 87403 Ae? 10 02 51.4627848072 -59 16 54.693903396   9.29 9.24     A1III 28 1
42 HD 95881 Em* 11 01 57.6218887080 -71 30 48.316074624   8.37 8.23     A0 101 0
43 HD 97048 Ae* 11 08 03.3109731720 -77 39 17.490777444 9.03 8.76 9.00   8.64 A0Vep 543 0
44 HD 98922 Be* 11 22 31.6743077592 -53 22 11.457008148   6.80 6.76     B9Ve 132 0
45 HD 100453 Ae* 11 33 05.5766482920 -54 19 28.547100696   8.09 7.79     F1Vn 285 1
46 HD 100546 Be* 11 33 25.4408872296 -70 11 41.241297948   6.71 6.30   6.64 A0VaekB8_lB 807 1
47 HD 101412 Be* 11 39 44.4564911064 -60 10 27.719780304   9.465 9.288     A3VaekA0mA0_lB 139 0
48 V* DX Cha Ae* 12 00 05.0868602544 -78 11 34.565724312   6.81 6.60     A4V 344 0
49 CD-40 8434 TT* 14 08 10.1545500744 -41 23 52.573291080   13.42 12.18 11.71 10.506 K7IVe 361 0
50 HD 132947 * 15 04 56.0564413224 -63 07 52.644571500   9.00 8.94     B9V 38 0
51 CPD-36 6759 Y*O 15 15 48.4460065200 -37 09 16.024369824   9.21 8.708     F8V 463 1
52 HD 139614 Ae? 15 40 46.3820275416 -42 29 53.538761832   8.47 8.24     A9VekA5mA5(_lB) 210 0
53 HD 141569 Y*O 15 49 57.7482550392 -03 55 16.341617064 7.22 7.20 7.12 7.00 7.04 A2VekB9mB9(_lB) 541 0
54 HD 142666 TT* 15 56 40.0221861696 -22 01 40.005872148 9.41 9.37 8.82 8.31 8.01 F0V_sh 269 0
55 HD 142527 Ae* 15 56 41.8882637904 -42 19 23.248281828   9.04 8.34     F6III 643 1
56 HD 143006 Or* 15 58 36.9126279888 -22 57 15.220559196   10.92 10.14   8.70 G5IVe 255 0
57 HD 144432 Ae* 16 06 57.9533126832 -27 43 09.760564056 8.47 8.53 8.19 7.82 7.53 A9/F0V 245 1
58 V* V856 Sco Ae* 16 08 34.2870044544 -39 06 18.325711332 7.66 7.41 7.05 6.92   A9V_sh 388 0
59 HD 145718 Ae* 16 13 11.5918435992 -22 29 06.621987516   9.29 8.86     A5Ve 113 0
60 HD 149914 * 16 38 28.6527873384 -18 13 13.713126384   6.967 6.746     B9.5IV 70 0
61 HD 150193 Ae* 16 40 17.9243127240 -23 53 45.193372692 9.69 9.32 8.79 8.41   A3Va(e) 321 0
62 * c Oph Be* 17 31 24.9538710166 -23 57 45.514802684 4.75 4.81 4.81 4.74 4.72 A0V 273 0
63 NAME Galactic Center reg 17 45 39.60213 -29 00 22.0000           ~ 14463 0
64 HD 163296 Ae* 17 56 21.2881851168 -21 57 21.871819008 7.00 6.93 6.85 6.86 6.67 A3VaekA1mA1 1113 0
65 HD 169142 Ae* 18 24 29.7799891464 -29 46 49.327400568   8.42 8.16     F1VekA3mA3_lB? 449 0
66 HD 176386 Y*O 19 01 38.9318002416 -36 53 26.561166432 7.28 7.44 7.32 8.11   B9Vbs 136 0
67 HD 179218 Ae* 19 11 11.2538919456 +15 47 15.636008472 7.55 7.476 7.39 7.25 7.21 A0Ve 255 0
68 V* WW Vul Ae* 19 25 58.7494120560 +21 12 31.333658616 11.46 10.99 10.25 10.38 10.12 A2IVe 224 0
69 V* PX Vul Or* 19 26 40.2532914312 +23 53 50.782579116 12.56 12.57 11.83 10.90 10.30 F3Ve 57 0
70 HD 190073 Ae* 20 03 02.5098474264 +05 44 16.660712904 7.91 7.86 7.73   7.65 A2IVe 256 0
71 V* DV Aqr SB* 20 58 41.8398627000 -14 28 59.250192924   6.192 5.963   6.010 A9V 91 0
72 V* BP Psc pA? 23 22 24.6974756088 -02 13 41.378919456   13.32 11.85     G9IIIe 48 0

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