2009A&A...502..283H


Query : 2009A&A...502..283H

2009A&A...502..283H - Astronomy and Astrophysics, volume 502, 283-301 (2009/7-4)

Searching for a link between the magnetic nature and other observed properties of Herbig Ae/Be stars and stars with debris disks.

HUBRIG S., STELZER B., SCHOELLER M., GRADY C., SCHUETZ O., POGODIN M.A., CURE M., HAMAGUCHI K. and YUDIN R.V.

Abstract (from CDS):

Recently, evidence for the presence of weak magnetic fields in Herbig Ae/Be stars has been found in several studies. We seek to expand the sample of intermediate-mass pre-main sequence stars with circular polarization data to measure their magnetic fields, and to determine whether magnetic field properties in these stars are correlated with mass-accretion rate, disk inclination, companions, silicates, PAHs, or show a correlation with age and X-ray emission as expected for the decay of a remnant dynamo. Spectropolarimetric observations of 21 Herbig Ae/Be stars and six debris disk stars have been obtained at the European Southern Observatory with FORS1 mounted on the 8m Kueyen telescope of the VLT. With the GRISM600B in the wavelength range 3250-6215Å we were able to cover all hydrogen Balmer lines from Hβ to the Balmer jump. In all observations a slit width of 0.4" was used to obtain a spectral resolving power of R≃2000. Among the 21 Herbig Ae/Be stars studied, new detections of a magnetic field were achieved in six stars. For three Herbig Ae/Be stars, we confirm previous magnetic field detections. The largest longitudinal magnetic field, <Bz≥-454±42G, was detected in the Herbig Ae/Be star HD101412 using hydrogen lines. No field detection at a significance level of 3σ was achieved in stars with debris disks. Our study does not indicate any correlation of the strength of the longitudinal magnetic field with disk orientation, disk geometry, or the presence of a companion. We also do not see any simple dependence on the mass-accretion rate. However, it is likely that the range of observed field values qualitatively supports the expectations from magnetospheric accretion models giving support for dipole-like field geometries. Both the magnetic field strength and the X-ray emission show hints of a decline with age in the range of ∼2-14Myr probed by our sample, supporting a dynamo mechanism that decays with age. However, our study of rotation does not show any obvious trend of the strength of the longitudinal magnetic field with rotation period. Furthermore, the stars seem to obey the universal power-law relation between magnetic flux and X-ray luminosity established for the Sun and main-sequence active dwarf stars.

Abstract Copyright:

Journal keyword(s): polarization - stars: pre-main-sequence - stars: circumstellar matter - stars: magnetic fields - X-rays: stars - stars: coronae

Simbad objects: 42

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Number of rows : 42
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 * 36 Psc ** 00 16 34.0418564136 +08 14 24.566106696   7.042 6.121     G8II-III 52 0
2 CD-53 251 Ae? 01 17 43.4985952032 -52 33 30.791840040   11.28 10.75     F3Ve 30 0
3 HD 6369 * 01 24 29.4579663912 +88 15 45.538991532   9.20 8.87     F5 10 0
4 * 49 Cet PM* 01 34 37.7786780856 -15 40 34.898673000   5.667 5.607   5.54 A1V 279 0
5 HD 31648 Ae* 04 58 46.2655706952 +29 50 36.987625680 7.84 7.78 7.62 7.76 7.43 A5Vep 474 0
6 BD-06 1253 Ae* 05 36 25.4320468080 -06 42 57.684730284   11.65 10.9 10.29   A1e 425 1
7 V* BF Ori Ae* 05 37 13.2623828280 -06 35 00.568242528 10.37 10.00 9.69 10.06 9.31 A7III 282 0
8 * bet Pic PM* 05 47 17.0876901 -51 03 59.441135 4.13 4.03 3.86 3.74 3.58 A6V 1814 1
9 * 15 Mon Be* 06 40 58.65963 +09 53 44.7229 3.360 4.45 4.68   4.88 O7V+B1.5/2V 781 0
10 NAME Cone Nebula DNe 06 41.1 +09 53           ~ 83 1
11 HD 85567 Be* 09 50 28.5375988920 -60 58 02.954048268 8.16 8.67 8.57     B5Vne 88 0
12 HD 95881 Em* 11 01 57.6218887080 -71 30 48.316074624   8.37 8.23     A0 94 0
13 NAME Cha 1 MoC 11 06 48 -77 18.0           ~ 1095 1
14 HD 97048 Ae* 11 08 03.3109731720 -77 39 17.490777444 9.03 8.76 9.00   8.64 A0Vep 515 0
15 HD 97300 Ae* 11 09 50.0199904704 -76 36 47.718191232   9.41 9.20   8.82 B9V 168 1
16 HD 98922 Be* 11 22 31.6743077592 -53 22 11.457008148   6.80 6.76     B9Ve 126 1
17 HD 100453 Ae* 11 33 05.5766482920 -54 19 28.547100696   8.09 7.79     A9Ve 254 1
18 HD 100546 Be* 11 33 25.4408872296 -70 11 41.241297948   6.71 6.30   6.64 A0VaekB8_lB 746 1
19 HD 101412 Be* 11 39 44.4564911064 -60 10 27.719780304   9.465 9.288     A3VaekA0mA0_lB 131 0
20 V* DX Cha Ae* 12 00 05.0868602544 -78 11 34.565724312   6.81 6.60     A0_sh 330 0
21 HD 109573 PM* 12 36 01.0317461592 -39 52 10.220465388   5.786 5.774 7.25 5.81 A0V 603 1
22 CPD-36 6759 Y*O 15 15 48.4460065200 -37 09 16.024369824   9.21 8.708     F8V 426 1
23 HD 135344 * 15 15 48.9462675744 -37 08 55.731368400   7.84 7.76     A0V 140 1
24 HD 139614 Ae? 15 40 46.3820275416 -42 29 53.538761832   8.47 8.24     A9VekA5mA5(_lB) 193 0
25 HD 144432 Ae* 16 06 57.9533126832 -27 43 09.760564056 8.47 8.53 8.19 7.82 7.53 A9/F0V 230 1
26 V* V856 Sco Ae* 16 08 34.2870044544 -39 06 18.325711332 7.66 7.41 7.05 6.92   A7IIIne_sh 375 0
27 HD 150193 Be* 16 40 17.9243127240 -23 53 45.193372692 9.69 9.32 8.79 8.41   B9.5Ve 307 0
28 V* AK Sco Ae* 16 54 44.8491575376 -36 53 18.566586456 9.80 9.63 9.00     F5V 259 1
29 CD-42 11721 Be* 16 59 06.7629322176 -42 42 08.404228224 12.16 12.28 11.00     B0IVe 164 0
30 * c Oph Be* 17 31 24.9538710166 -23 57 45.514802684 4.75 4.81 4.81 4.74 4.72 A0V 266 0
31 V* V951 Sco a2* 17 53 58.1358478008 -34 49 51.800052684   6.43 6.42     kB6hA0VHeA0pSiCr 98 0
32 HD 163296 Ae* 17 56 21.2881851168 -21 57 21.871819008 7.00 6.93 6.85 6.86 6.67 A1Vep 1003 0
33 HD 164249 PM* 18 03 03.4097283792 -51 38 56.432149872   7.438 7.007 7.90   F6V 112 0
34 HD 169142 Ae* 18 24 29.7799891464 -29 46 49.327400568   8.42 8.16     F1VekA3mA3_lB? 409 2
35 EM* MWC 297 Ae* 18 27 39.5265500160 -03 49 52.133050776 15.57 14.34 12.31 11.34   B1.5Ve 286 0
36 V* VV Ser Ae* 18 28 47.8620017808 +00 08 39.923474964 12.99 12.63 11.80 11.01 10.24 A5Ve 242 0
37 HD 172555 PM* 18 45 26.9009806435 -64 52 16.534807985   4.967 4.767     A7V 263 0
38 HD 176386 Y*O 19 01 38.9318002416 -36 53 26.561166432 7.28 7.44 7.32 8.11   B9V 128 0
39 HD 179218 Ae* 19 11 11.2538919456 +15 47 15.636008472 7.55 7.476 7.39 7.25 7.21 A0Ve 241 0
40 HD 181327 PM* 19 22 58.9437222504 -54 32 16.975668624   7.50 7.04   6.49 F6V 268 0
41 HD 190073 Ae* 20 03 02.5098474264 +05 44 16.660712904 7.91 7.86 7.73   7.65 A2IVe 244 0
42 HD 200775 Ae* 21 01 36.9205762896 +68 09 47.789578836 7.34 7.754 7.427 8.13   B2Ve 539 0

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2023.02.04-20:06:07

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