2009A&A...499..579B


C.D.S. - SIMBAD4 rel 1.7 - 2020.08.09CEST08:03:29

2009A&A...499..579B - Astronomy and Astrophysics, volume 499, 579-593 (2009/5-4)

The young active star SAO51891 (V383 Lacertae).

BIAZZO K., FRASCA A., MARILLI E., COVINO E., ALCALA J.M., CAKIRLI O., KLUTSCH A. and MEYER M.R.

Abstract (from CDS):

The aim of this work is to investigate the surface inhomogeneities of a young, late-type star, SAO51891, at different atmospheric levels, from the photosphere to the upper chromosphere, analyzing contemporaneous optical high-resolution spectra and broad-band photometry. The full spectral range of FOCESAHA (R≃40000) is used to perform the spectral classification and to determine the rotational and radial velocities. The lithium abundance is measured to obtain an age estimate. The BVRIJHKs photometric bands are used to construct the spectral energy distribution (SED). The variations in the observed BV fluxes and effective temperature are used to infer the presence of photospheric spots and observe their behavior over time. The chromospheric activity is studied applying the spectral subtraction technique to Hα, CaII H&K, Hε, and CaII IRT lines. We find SAO51891 to be a young K0-1V star with a lithium abundance close to the Pleiades upper envelope, confirming its youth (∼100Myr), which is also inferred from its kinematical membership of the Local Association. No infrared excess is detected from analysis of its SED, limiting the amount of remaining circumstellar dust. We detect a rotational modulation of the luminosity, effective temperature, CaII H&K, Hε, and CaII IRT total fluxes. A simple spot model with two main active regions, about 240K cooler than the surrounding photosphere, fits the observed light and temperature curves very well. The small-amplitude radial velocity variations are also well reproduced by our spot model. The anti-correlation of light curves and chromospheric diagnostics indicates chromospheric plages spatially associated with the spots. The largest modulation amplitude is observed for the Hε flux suggesting that this line is very sensitive to the presence of chromospheric plages. SAO51891 is a young active star, lacking significant amounts of circumstellar dust or any evidence of low mass companions, and displays the typical phenomena produced by magnetic activity. The spots are larger and warmer than those in less active main-sequence stars. If some debris is still present around the star, it will only be detectable by future far-infrared and sub-mm observations (e.g., Herschel or ALMA). The RV variation produced by the starspots has an amplitude comparable with those induced by Jupiter-mass planets orbiting close to the host star. SAO51891 is another good example of an active star in which the detection of planets may be hampered by the high activity level.

Abstract Copyright:

Journal keyword(s): stars: fundamental parameters - stars: activity - stars: late-type - stars: planetary systems: protoplanetary disks - starsi: individual: SAO 51891

Simbad objects: 22

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Number of rows : 22

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#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 526 1
2 HD 12028 * 01 58 58.4705492960 +37 08 14.781888325   9.18 8.73     F5V 9 0
3 * alf Ari PM* 02 07 10.40570 +23 27 44.7032 4.29 3.17 2.01 1.15 0.54 K2-IIIbCa-1 604 1
4 * kap01 Cet BY* 03 19 21.6963205 +03 22 12.715139 5.71 5.52 4.85 4.27 3.91 G5V 824 0
5 Cl Melotte 22 OpC 03 47 00 +24 07.0           ~ 2990 0
6 Cl Melotte 25 OpC 04 26 54.00 +15 52 00.0           ~ 2664 0
7 HD 31392 PM* 04 54 04.2086268739 -35 24 16.263393746   8.40 7.61     G9V 68 0
8 HD 32147 PM* 05 00 48.9991346145 -05 45 13.220341956 8.27 7.27 6.21 5.36 4.87 K3+V 415 1
9 NGC 1901 OpC 05 18 11 -68 27.0           ~ 77 0
10 NGC 2632 OpC 08 40 24 +19 40.0           ~ 1232 0
11 IC 2391 OpC 08 40 32 -53 02.0           ~ 717 0
12 BD+20 2465 Er* 10 19 36.2808024653 +19 52 12.014037746   10.82 9.52 9.19   M4Vae 1152 0
13 NAME Coma Dwarf Galaxy G 12 26 59.0 +23 54 15     14.1     ~ 391 1
14 NAME Ursa Major Moving Group MGr 12 32 +57.0           ~ 379 2
15 NAME NGP reg 12 51 26.275 +27 07 41.70           ~ 1023 0
16 * alf Boo RG* 14 15 39.67207 +19 10 56.6730 2.46 1.18 -0.05 -1.03 -1.68 K1.5IIIFe-0.5 2136 0
17 * alf Aql dS* 19 50 46.99855 +08 52 05.9563 1.07 0.98 0.76 0.62 0.49 A7Vn 820 0
18 V* HN Peg BY* 21 44 31.3299733695 +14 46 18.982331039       6.16   G0V+ 452 0
19 BD+48 3666 PM* 22 17 26.8789565317 +49 11 44.765252940   8.80 8.28     F8 11 0
20 V* V383 Lac BY* 22 20 07.0254836275 +49 30 11.763794475   9.42 8.58     K1V 72 0
21 NAME Pleiades Moving Group MGr ~ ~           ~ 239 1
22 NAME Castor Moving Group As* ~ ~           ~ 116 1

    Equat.    Gal    SGal    Ecl

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2020.08.09-08:03:29

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