2001PASP..113..188P

Query : 2001PASP..113..188P

2001PASP..113..188P - Publ. Astron. Soc. Pac., 113, 188-194 (2001/February-0)

A large spectral class dependence of the Wilson-Bappu effect among luminous stars.

PARSONS S.B.

Abstract (from CDS):

The striking correlation between Ca II K-line emission width and absolute visual magnitude has not previously been well calibrated for stars more luminous than giants. From a sample of binary systems fit to isochrones, we find deviations of more than 2 mag, correlated with spectral class, between these binarity Mv values and the Wilson-Bappu relation. Additional Mv values derived from Hipparcos parallaxes are used to explore the systematics. The spectral class dependence vanishes for K-line parameter logW0≤1.80. Linear spectral class corrections are derived for the more luminous stars, with logW0≥2.00, while a table is provided for the transition region. The dispersion from these relations is about ±0.6 mag. This recalibration extends the demonstrated applicability of the Wilson-Bappu technique to Mv≃-5 or distance ~20 kpc.

Abstract Copyright: ∼

Journal keyword(s): Stars: Binaries: Spectroscopic - Stars: Chromospheres - Stars: Distances - Stars: Fundamental Parameters - Stars: Late-Type - Stars: Supergiants

Simbad objects: 24

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Number of rows : 24
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 V* KK Per s*r 02 10 15.7846748496 +56 33 32.663347416 12.32 9.96 7.74 5.86 4.29 M2Iab-Ib 108 0
2 V* AD Per s*r 02 20 29.0035384536 +56 59 35.239755912 12.70 10.16 7.8490   7.1111 M3Iab 129 1
3 V* PR Per s*r 02 21 42.4097766240 +57 51 46.144950588 12.84 10.31 8.00 6.13 4.60 M1-Iab-Ib 122 0
4 * mu. Per SB* 04 14 53.8635146524 +48 24 33.590334394 5.75 5.12 4.16 3.38 2.83 G0Ib 252 0
5 * zet Aur SB* 05 02 28.6834429313 +41 04 32.995159760 5.35 4.97 3.75 2.62 1.75 K5II+B7V 470 0
6 * pi. Pup LP* 07 17 08.5580780520 -37 05 50.904468727 5.57 4.32 2.70 1.46 0.55 K4III 116 0
7 HD 57146 * 07 18 51.2737383648 -26 35 09.081112236   6.258 5.288     G2Ib 86 0
8 * c Pup * 07 45 15.2961339331 -37 58 06.906935781 7.06 5.34 3.61 2.26 1.26 K4III 107 0
9 * eps Car ** 08 22 30.83526 -59 30 34.1431 3.32 3.13 1.86     K3:III+B2:V 98 0
10 * F Hya * 08 43 40.3744846779 -07 14 01.422508229   5.441 4.625     G1Ib 172 0
11 * alf UMa ** 11 03 43.67152 +61 45 03.7249 3.78 2.86 1.79 0.98 0.40 G9III+A7.5 448 0
12 V* V810 Cen LP* 11 43 31.1923164072 -62 29 21.827165856 6.18 5.83 5.03 4.27 3.91 G0_0-IaFe1 158 0
13 * 21 Sgr * 18 25 21.0394302144 -20 32 30.022206936   6.32 4.86     K1/2III 65 0
14 * bet Sct SB* 18 47 10.4742156840 -04 44 52.342960488 6.15 5.31 4.22 3.43 2.86 G4IIa 194 0
15 * nu.01 Sgr * 18 54 10.1780830272 -22 44 41.422617132   6.251 4.845     K1II 101 0
16 * del Sge SB* 19 47 23.2655973192 +18 32 03.528856248 6.20 5.12 3.81 2.37 1.08 M2II+B0V 208 0
17 * 31 Cyg SB* 20 13 37.9082370480 +46 44 28.761618048 5.50 5.08 3.80 2.83 2.07 K3Ib+B2IV-V 385 0
18 * omi02 Cyg SB* 20 15 28.3242122880 +47 42 51.213932496 6.54 5.50 3.98 2.78 1.86 K7Ib-II+B1V 347 0
19 * 22 Vul SB* 20 15 30.2386386720 +23 30 32.051069712   6.192 5.176     G3Ib-II 215 0
20 * 49 Cyg ** 20 41 02.5422151056 +32 18 26.238680208   6.672 5.638     G8IIb 89 0
21 * ksi Cyg SB* 21 04 55.8599363125 +43 55 40.272058234 7.17 5.39 3.73 2.55 1.63 K4.5Ib-II 324 0
22 * 5 Lac s*r 22 29 31.8281552924 +47 42 24.861238614 7.15 6.05 4.37 2.98 1.91 K9Ia+B2V 152 0
23 * eta Peg SB* 22 43 00.1288449480 +30 13 16.372969392 4.38 3.81 2.95 2.31 1.83 G8II+F0V 208 0
24 * psi And ** 23 46 02.0470343064 +46 25 12.986458896   6.064 4.966     G3Ib-II 188 0

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