1998A&A...339..840S

Query : 1998A&A...339..840S

1998A&A...339..840S - Astronomy and Astrophysics, volume 339840-845 (1998/11-3)

The relation between the magnetic field strength and the coronal temperature of cool stars.

SHI J.R., ZHAO G., ZHAO Y.-H. and YOU J.-H.

Abstract (from CDS):

The correlation between the coronal X-ray temperature and the magnetic field strength in late-type stars is investigated, based on data primarily from the ROSAT PSPC. According to the observation, we divide the stars into three groups: single, binary and RS CVn stars. From the sample of single stars, we find a clear correlation of the coronal temperature with the magnetic field strength. We interpret that result as the magnetic heating process.

Abstract Copyright: ∼

Journal keyword(s): stars: activity - stars: coronae - stars: late-type - stars: magnetic fields - X-rays: stars

Simbad objects: 30

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Number of rows : 30
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 HD 166 BY* 00 06 36.7840068588 +29 01 17.412693890   6.82 6.07 5.6   G8V 392 0
2 * 9 Cet BY* 00 22 51.7884553555 -12 12 33.969921319 7.29 7.05 6.39     G2.5V 510 0
3 * 107 Psc PM* 01 42 29.7625251280 +20 16 06.645657710 6.57 6.08 5.24 4.55 4.12 K1V 594 0
4 V* VY Ari RS* 02 48 43.7287198695 +31 06 54.592461256   7.72   6.4   G9 241 0
5 HD 17925 RS* 02 52 32.1281856011 -12 46 10.968056223 7.48 6.91 6.05 5.34 4.89 K1V 557 0
6 * kap01 Cet BY* 03 19 21.6964175772 +03 22 12.714979884 5.71 5.52 4.85 4.27 3.91 G5V 948 0
7 * eps Eri BY* 03 32 55.8444911587 -09 27 29.739493865 5.19 4.61 3.73 3.00 2.54 K2V 2073 1
8 HD 22468 RS* 03 36 47.2904292073 +00 35 15.943692002 7.09 6.79 5.90     K2:Vnk 1206 0
9 HD 283750 BY* 04 36 48.2421502608 +27 07 55.888214520   9.19 8.10 7.4   K2.5Ve 289 0
10 HD 36395 PM* 05 31 27.3957852161 -03 40 38.024004501 10.626 9.443 7.968 6.996 5.913 M1.5Ve 574 0
11 * chi01 Ori SB* 05 54 22.9829893 +20 16 34.222038 5.08 5.00 4.40 3.90 3.59 G0V 895 0
12 HD 45088 BY* 06 26 10.2546417144 +18 45 24.761018520 8.402 7.74   6.2   K2Ve 255 0
13 * sig Gem RS* 07 43 18.7276907303 +28 53 00.631838445 6.38 5.41 4.29 3.37 2.79 K1IIIe 499 0
14 V* AD Leo PM* 10 19 36.2808181226 +19 52 12.010446571   10.82 9.52 9.19   dM3 1469 1
15 * 61 UMa PM* 11 41 03.0162706212 +34 12 05.881605449 6.31 6.08 5.34 4.73 4.38 G8V 654 0
16 HD 115404 PM* 13 16 51.0514297623 +17 01 01.840901307   7.69 6.66     K2V 316 0
17 HD 118100 PM* 13 34 43.2063495866 -08 20 31.338030204 11.578 10.552 9.372 8.602 7.930 K5Ve 360 0
18 * alf Cen A SB* 14 39 36.49400 -60 50 02.3737 0.96 0.72 0.01     G2V 1352 1
19 * ksi Boo BY* 14 51 23.37993 +19 06 01.6994 5.618 5.370 4.593 3.91 3.48 G7Ve+K5Ve 503 0
20 V* DE Boo RS* 14 53 23.7654730144 +19 09 10.072718521   6.84 6.00 5.5   K0.5V 287 0
21 HD 131977 BY* 14 57 28.0007918772 -21 24 55.727265310 7.89 6.83 5.72 4.74 4.19 K4V 525 0
22 HD 152391 PM* 16 52 58.8025159848 -00 01 35.118396116   7.40 6.64     G8.5Vk: 396 0
23 HD 152751 ** 16 55 28.7575690 -08 20 10.787849 11.647 10.593 9.023 7.937 6.565 M3.5Ve 547 1
24 * 70 Oph SB* 18 05 27.28518 +02 30 00.3558 5.40 4.89 4.03 3.38 2.92 K0-V 679 0
25 * sig Dra PM* 19 32 21.5902098601 +69 39 40.235805206 5.860 5.460 4.680 4.04 3.63 K0V 691 0
26 * 61 Cyg A BY* 21 06 53.9395895022 +38 44 57.902349973 7.50 6.39 5.21 4.19 3.54 K5V 1099 0
27 * eps Ind PM* 22 03 21.6536261624 -56 47 09.522795714   5.75 4.69     K5V 616 0
28 * lam And RS* 23 37 33.8427800830 +46 27 29.344721109 5.54 4.84 3.82 3.04 2.47 G8IVk 693 0
29 HD 224085 RS* 23 55 04.0520383542 +28 38 01.245426862 8.88 8.20   6.9   K2+IVeFe-1 756 0
30 V* DQ Psc LP* 23 59 46.4915508816 -00 16 48.404033940   8.45 6.84     M1III 24 0

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