2002A&A...394.1009C


C.D.S. - SIMBAD4 rel 1.7 - 2020.12.04CET19:30:16

2002A&A...394.1009C - Astronomy and Astrophysics, volume 394, 1009-1021 (2002/11-2)

Measuring starspot temperature from line depth ratios. I. The method.

CATALANO S., BIAZZO K., FRASCA A. and MARILLI E.

Abstract (from CDS):

Gray and collaborators have recently demonstrated that line-depth ratios are a powerful tool for temperature discrimination, able to resolve differences ≤10K. The method has been applied to detect temperature variations in the 5-15K range due to activity cycles (e.g. Gray et al., 1996ApJ...456..365G and 1996ApJ...465..945G) or to rotation modulation produced by large surface features, called ``star-patches", like that detected in ξ BooA by Toner & Gray (1988ApJ...334.1008T). Cool starspots of a few tenths of the stellar surface produce bumps in a line profile, which migrate through the line profile allowing Doppler-imaging in fast rotating stars. In the hypothesis that in slowly-rotating stars the passage of dark spots produces modulation of the center line depth of different amount in lines of different sensitivity to temperature, we have made test observations on three active binaries of the RS CVn type. Based on observations made at the Catania Astrophysical Observatory at a resolution R=14000, we show that line-depth ratios can be effectively used to determine spot temperatures of active binary systems. Using, on average, ten line pairs, selected in the 6100-6300Å wavelength range, with the help of observations of 30 main sequence and giant stars, we have derived a calibration relation of line-depth ratios (LDR) in an absolute temperature scale, taking into account the gravity effect in the calibration relation. Single LDRs converted to temperature through the calibration relations have led to clear rotational modulation of the average surface temperature with amplitudes of 177K, 119K, and 127K for VY Ari, IM Peg and HK Lac, with average estimated errors of about 10 K. We show that the observed temperature variation amplitude allows us to define a minimum fractional spotted area coverage as a function of spot-photosphere temperature ratio. Adopting the maximum value of average temperature, determined from the LDRs, as that of the unspotted photosphere, we computed the average spot temperature corresponding to the minimum spot coverage. Although not univocally constrained, the temperature difference (ΔT=Tph-Tsp) obtained for the three systems, ΔT=890K for VY Ari, ΔT=750K for IM Peg, and ΔT=810K for HK Lac, are in good agreement with values derived with other methods.

Abstract Copyright:

Journal keyword(s): stars: late-type - stars: activity - stars: starspots - stars: individual: VY Ari, HK Lac, IM Peg

Simbad objects: 33

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Number of rows : 33

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 * 54 Psc PM* 00 39 21.8055114029 +21 15 01.716052732 7.29 6.71 5.88 5.21 4.82 K0.5V 532 1
2 * tau Cet PM* 01 44 04.0834226 -15 56 14.926552 4.43 4.22 3.50 2.88 2.41 G8V 1107 1
3 * alf Ari PM* 02 07 10.40570 +23 27 44.7032 4.29 3.17 2.01 1.15 0.54 K2-IIIbCa-1 607 1
4 HD 16160 PM* 02 36 04.9023844802 +06 53 12.431588708   6.81   5.2   K3V 488 1
5 V* VY Ari RS* 02 48 43.7283572894 +31 06 54.592580835   7.72   6.4   G9 207 0
6 * kap01 Cet BY* 03 19 21.6963205 +03 22 12.715139 5.71 5.52 4.85 4.27 3.91 G5V 827 0
7 * eps Eri BY* 03 32 55.8449634 -09 27 29.731165 5.19 4.61 3.73 3.00 2.54 K2V 1721 1
8 * 10 Tau PM* 03 36 52.1448022536 +00 23 58.536917738 5.23 5.15 4.30 4.09 3.77 F9IV-V 527 0
9 * 12 Tau * 03 39 51.1214818739 +03 03 24.714360191   6.483 5.555     K0III 52 0
10 * del Eri RS* 03 43 14.9008787 -09 45 48.208444 5.13 4.46 3.54 2.82 2.32 K0+IV 548 0
11 * pi. Tau * 04 26 36.3717811513 +14 42 49.629139596 6.39 5.67 4.69 3.97 3.46 G7IIIFe-0.5 98 0
12 * alf Tau LP? 04 35 55.23907 +16 30 33.4885 4.32 2.40 0.86 -0.37 -1.31 K5+III 1188 1
13 * gam Mon * 06 14 51.3336645 -06 16 29.188011 6.69 5.27 3.96 2.99 2.36 K1III: 98 0
14 * 17 Mon * 06 47 19.8294628711 +08 02 14.123889454 7.82 6.17 4.77 3.74 3.04 K4III 111 0
15 * tau Gem ** 07 11 08.3704210 +30 14 42.583108 7.08 5.68 4.42 3.45 2.82 K2III 142 1
16 * ups Gem PM* 07 35 55.3506173748 +26 53 44.711452380 7.54 5.60 4.06 2.82 1.91 M0III 193 0
17 * kap Gem ** 07 44 26.8535692 +24 23 52.787227 5.19 4.49 3.57 2.86 2.41 G8III-IIIb 286 0
18 * bet Cnc PM* 08 16 30.9210081 +09 11 07.957924 6.750 5.000 3.520 2.42 1.62 K4IIIBa0.5: 344 0
19 * del Cnc ** 08 44 41.0992106 +18 09 15.503395 6.01 5.02 3.94 3.16 2.62 K0+IIIb 190 0
20 * w Her PM* 17 20 39.5675395123 +32 28 03.877348066 6.08 6.01 5.39 4.89 4.56 G0V 424 0
21 * 84 Her PM* 17 43 21.5646072179 +24 19 40.157353689   6.394 5.729     G2IIIb 136 0
22 * mu.01 Her ** 17 46 27.5266778 +27 43 14.437984 4.56 4.17 3.42 2.89 2.51 G5IV 654 0
23 * 16 Cyg A ** 19 41 48.9539315338 +50 31 30.218780803 6.79 6.59 5.95 5.50 5.17 G1.5Vb 679 1
24 * omi Aql PM* 19 51 01.6437560393 +10 24 56.595177367   5.66   4.8   F8V 425 0
25 * bet Aql PM* 19 55 18.7925630 +06 24 24.342501 5.040 4.560 3.710 3.05 2.56 G8IV 516 0
26 * kap Del PM* 20 39 07.7860368187 +10 05 10.279480343   5.77   4.6   G2IV 184 0
27 * eps Cyg ** 20 46 12.6823609 +33 58 12.924926 4.370 3.520 2.480 1.73 1.19 K0III 481 0
28 * 61 Cyg A BY* 21 06 53.9396100677 +38 44 57.897024357 7.50 6.39 5.21 4.19 3.54 K5V 952 0
29 * 61 Cyg B Er* 21 06 55.2640651855 +38 44 31.362140913 8.63 7.40 6.03 4.86 3.55 K7V 672 1
30 V* HK Lac RS* 22 04 56.6089126762 +47 14 04.482220545   8.01 6.96     K0III 230 0
31 * mu. Peg PM* 22 50 00.1931506 +24 36 05.698380 5.10 4.42 3.48 2.80 2.33 G8+III 278 0
32 V* IM Peg RS* 22 53 02.2658951462 +16 50 28.291474642   7.024 5.890     K2III 320 1
33 * 51 Peg Ro* 22 57 27.9804167474 +20 46 07.782240714 6.39 6.16 5.46 4.97 4.61 G2IV 1080 1

    Equat.    Gal    SGal    Ecl

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2020.12.04-19:30:16

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