2016ApJ...816...50R

Query : 2016ApJ...816...50R

2016ApJ...816...50R - Astrophys. J., 816, 50 (2016/January-2)

Magnetic grain trapping and the hot excesses around early-type stars.

RIEKE G.H., GASPAR A. and BALLERING N.P.

Abstract (from CDS):

A significant fraction of main sequence stars observed interferometrically in the near-infrared have slightly extended components that have been attributed to very hot dust. To match the spectrum appears to require the presence of large numbers of very small (<200 nm in radius) dust grains. However, particularly for the hotter stars, it has been unclear how such grains can be retained close to the star against radiation pressure force. We find that the expected weak stellar magnetic fields are sufficient to trap nm-sized dust grains in epicyclic orbits for a few weeks or longer, sufficient to account for the hot excess emission. Our models provide a natural explanation for the requirement that the hot excess dust grains be smaller than 200 nm. They also suggest that magnetic trapping is more effective for rapidly rotating stars, consistent with the average vsini measurements of stars with hot excesses being larger (at ∼2σ) than those for stars without such excesses. Universe

Abstract Copyright: ∼

Journal keyword(s): circumstellar matter - infrared: planetary systems - methods: numerical

Simbad objects: 51

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Number of rows : 51
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 * kap Phe PM* 00 26 12.2013436436 -43 40 47.390371480 4.22 4.11 3.94 3.78 3.70 A5IVn 158 0
2 * lam02 Phe PM* 00 35 41.1754684944 -48 00 03.264963408   5.948 5.510     F5V+ 77 0
3 * del Hyi PM* 02 21 44.9423652192 -68 39 33.906922488 4.17 4.12 4.09 4.05 4.04 A2V 119 0
4 * sig Cet ** 02 32 05.1877984910 -15 14 41.653561505 5.19 5.20 4.75 4.34 4.07 F5V 217 0
5 * kap Ret PM* 03 29 22.6774206459 -62 56 15.104181615   5.09 4.70     F3IV/V 184 0
6 * 10 Tau PM* 03 36 52.3837044168 +00 24 05.992097829 5.23 5.15 4.30 4.09 3.77 F9IV-V 595 0
7 * c Tau BS? 04 38 09.4618938672 +12 30 39.013056648 4.52 4.39 4.27 4.13 4.08 A6V 207 0
8 * pi.03 Ori PM* 04 49 50.4112051485 +06 57 40.600622266 3.620 3.630 3.190 2.77 2.51 F6V 601 0
9 HD 30781 * 04 50 27.8687073816 -03 51 54.751366368   8.55 7.36     K0III 13 0
10 * zet Lep * 05 46 57.3413646658 -14 49 19.020570470   3.637 3.525     A2IV-V(n) 308 0
11 * bet Pic PM* 05 47 17.0876901 -51 03 59.441135 4.13 4.03 3.86 3.74 3.58 A6V 2087 1
12 * eta Lep PM* 05 56 24.2934904501 -14 10 03.718335613 4.05 4.05 3.72 3.39 3.23 F2V 352 0
13 * alf CMa SB* 06 45 08.91728 -16 42 58.0171 -1.51 -1.46 -1.46 -1.46 -1.43 A0mA1Va 1610 0
14 * ksi Gem RG* 06 45 17.3644854477 +12 53 44.141855267 3.85 3.79 3.36 2.97 2.74 F5IV-V 233 0
15 * 30 Mon PM* 08 25 39.6318651278 -03 54 23.137987255 3.85 3.88 3.90 3.87 3.92 A0Va 289 0
16 * q Vel PM* 10 14 44.1556880397 -42 07 18.988830783 3.98 3.90 3.85 3.83 3.81 A2Va 146 0
17 * bet UMa PM* 11 01 50.4797515135 +56 22 56.761138187 2.35 2.35 2.37 2.31 2.35 A1IVps 462 0
18 * del Leo PM* 11 14 06.50142 +20 31 25.3853 2.79 2.68 2.53 2.44 2.41 A5IV(n) 292 0
19 * bet Leo dS* 11 49 03.57834 +14 34 19.4090 2.30 2.22 2.13 2.08 2.06 A3Va 605 1
20 HD 104731 PM* 12 03 39.5724147833 -42 26 02.610414638 5.53 5.56 5.15     F5V 144 0
21 * del UMa PM* 12 15 25.5598467041 +57 01 57.421119850 3.460 3.410 3.320 3.25 3.25 A2Vn 312 0
22 * del Crv PM* 12 29 51.8551642 -16 30 55.552542 2.80 2.89 2.94 2.99 3.03 A0IV(n)kB9 218 0
23 * tau Cen PM* 12 37 42.1640998080 -48 32 28.699293408 3.94 3.91 3.86 3.81 3.77 A1IVnn 113 0
24 * tau Boo PM* 13 47 15.7381720026 +17 27 24.809555600 5.02 4.98 4.49 4.09 3.85 F7IV-V 1049 1
25 * sig Boo PM* 14 34 40.8173867232 +29 44 42.457673940 4.76 4.84 4.47 4.13 3.94 F4VkF2mF1 632 0
26 * alf Cir a2* 14 42 30.4206520931 -64 58 30.478845491 3.55 3.43 3.19 2.96 2.86 A7VpSrCrEu 384 0
27 * mu. Vir PM* 14 43 03.6239867612 -05 39 29.524956308 4.25 4.26 3.88 3.48 3.26 F2V 239 0
28 * c Boo PM* 15 07 18.0659348352 +24 52 09.099406380 5.34 5.36 4.93 4.53 4.32 F5V 374 0
29 * bet Cir PM* 15 17 30.8494520580 -58 48 04.345266926   4.153 4.057     A3Va 136 0
30 * g Lup PM* 15 41 11.3768069149 -44 39 40.341696305   5.036 4.633     F4V 212 0
31 * gam Ser PM* 15 56 27.1826577018 +15 39 41.809580382 4.31 4.34 3.84 3.37 3.13 F6V 586 0
32 HD 143956 * 16 04 00.2383602864 -19 46 02.926413336   7.91 7.77     B9Van 63 0
33 * lam Ara PM* 17 40 23.8255785576 -49 24 56.099256516   5.17 4.77     F4V 132 0
34 * gam Oph PM* 17 47 53.5605898827 +02 42 26.204838837 3.83 3.80 3.75 3.71 3.71 A1VnkA0mA0 411 0
35 * zet Ser PM* 18 00 29.0100539320 -03 41 24.977568563   4.982 4.616     F2V 203 0
36 * 72 Oph PM* 18 07 20.9848472070 +09 33 49.848215907 3.95 3.85 3.73 3.59 3.54 A5V 156 0
37 * alf Lyr dS* 18 36 56.33635 +38 47 01.2802 0.03 0.03 0.03 0.07 0.10 A0V 2787 1
38 * 110 Her PM* 18 45 39.7256792847 +20 32 46.713086264 4.66 4.65 4.19 3.80 3.54 F5.5IV-V 427 0
39 * zet Aql PM* 19 05 24.6080155 +13 51 48.518212 2.99 3.00 2.99 2.98 2.98 A0IV-Vnn 364 0
40 * alf CrA PM* 19 09 28.3415149600 -37 54 16.107840507   4.146 4.087     A2Va 120 0
41 HD 226099 SB* 19 50 40.9318420579 +34 57 00.224167823       7.5   G5 32 0
42 * alf Aql dS* 19 50 46.99855 +08 52 05.9563 1.07 0.98 0.76 0.62 0.49 A7Vn 919 1
43 * eps Pav PM* 20 00 35.5515303087 -72 54 37.812955563   3.927 3.940     A0Va 142 0
44 * eta Ind dS* 20 44 02.3339803529 -51 55 15.493271117   4.767 4.495     A9IV 93 0
45 * psi Cap PM* 20 46 05.7329952443 -25 16 15.233491015   4.538 4.122     F5V 230 0
46 * alf Cep PM* 21 18 34.77233 +62 35 08.0681 2.770 2.680 2.460 2.22 2.11 A8Vn 374 0
47 * mu. PsA PM* 22 08 23.0113421424 -32 59 18.491668224 4.60 4.55 4.50 4.43 4.38 A1.5IVn 132 0
48 * tau PsA PM* 22 10 08.7801946925 -32 32 54.270294310   5.40 4.92     F6V 175 0
49 * eps Cep SB* 22 15 02.1972987635 +57 02 36.846735569   4.47   4.0   F0V(Sr) 237 0
50 * ups Aqr PM* 22 34 41.6357860992 -20 42 29.576916972   5.637 5.203     F7V 148 0
51 * alf PsA PM* 22 57 39.04625 -29 37 20.0533 1.31 1.25 1.16 1.11 1.09 A4V 1303 3

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