2020A&A...643A..39C


Query : 2020A&A...643A..39C

2020A&A...643A..39C - Astronomy and Astrophysics, volume 643A, 39-39 (2020/11-1)

Magnetic field and prominences of the young, solar-like, ultra-rapid rotator V530 Persei.

CANG T.-Q., PETIT P., DONATI J.-F., FOLSOM C.P., JARDINE M., VILLARREAL D'ANGELO C., VIDOTTO A.A., MARSDEN S.C., GALLET F. and ZAIRE B.

Abstract (from CDS):


Context. Young solar analogs reaching the main sequence experience very strong magnetic activity, generating angular momentum losses through wind and mass ejections.
Aims. We investigate signatures of magnetic fields and activity at the surface and in the prominence system of the ultra-rapid rotator V530 Per, a G-type solar-like member of the young open cluster α Persei. This object has a rotation period that is shorter than all stars with available magnetic maps.
Methods. With a time-series of spectropolarimetric observations gathered with ESPaDOnS over two nights on the Canada-France-Hawaii Telescope, we reconstructed the surface brightness and large-scale magnetic field of V530 Per using the Zeeman-Doppler imaging method, assuming an oblate stellar surface. We also estimated the short term evolution of the brightness distribution through latitudinal differential rotation. Using the same data set, we finally mapped the spatial distribution of prominences through tomography of the Hα emission.
Results. The brightness map is dominated by a large, dark spot near the pole, accompanied by a complex distribution of bright and dark features at lower latitudes. Taking the brightness map into account, the magnetic field map is reconstructed as well. Most of the large-scale magnetic field energy is stored in the toroidal field component. The main radial field structure is a positive region of about 500 G, at the location of the dark polar spot. The brightness map of V530 Per is sheared by solar-like differential rotation, with roughly a solar value for the difference in rotation rate between the pole and equator. It is important to note that Hα is observed in emission and it is mostly modulated by the stellar rotation period over one night. The prominence system is organized in a ring at the approximate location of the corotation radius, and displays significant evolution between the two observing nights.
Conclusions. V530 Per is the first example of a solar-type star to have its surface magnetic field and prominences mapped together, which will bring important observational constraints to better understand the role of slingshot prominences in the angular momentum evolution of the most active stars.

Abstract Copyright: © T.-Q. Cang et al. 2020

Journal keyword(s): stars: individual: V530 Per - stars: magnetic field - stars: solar-type - stars: rotation - starspots

Status at CDS : Objects in title, abstract, text, figures, and all or part of small table(s) being processed in SIMBAD.

Simbad objects: 22

goto Full paper

goto View the references in ADS

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 - 2023
#notes
1 V* CC Eri BY* 02 34 22.5661889568 -43 47 46.869120096 11.305 10.201 8.865 7.926 6.992 K7V 261 0
2 ACO 426 ClG 03 19 47.2 +41 30 47           ~ 2149 1
3 V* V484 Per BY* 03 22 21.9201012551 +49 08 27.732216837   12.07 11.37     G6V 60 0
4 V* V530 Per BY* 03 24 48.3831600744 +48 53 19.834031868   12.53       G8V 28 0
5 V* V532 Per BY* 03 26 22.2275044296 +49 25 37.501937904   11.98 11.27     G2-3V 61 0
6 V* V689 Per BY* 03 32 10.2250397496 +49 08 28.764388392   13.13 11.99     G5V 24 0
7 HD 22468 RS* 03 36 47.2911034958 +00 35 15.938962144 7.09 6.79 5.90 5.4   K2:Vnk 1152 0
8 V* V1038 Tau BY* 03 44 20.0898026175 +24 47 46.205031064   11.2 10.4 10.3   G1-2V 124 0
9 EM* LkCa 4 Or* 04 16 28.1067298272 +28 07 35.731363080   13.96 12.78 11.825   K7:Ve 170 0
10 V* V410 Tau Or* 04 18 31.1081296680 +28 27 16.155955728   12.13 10.75 8.45 9.408 K3Ve 447 0
11 V* V1069 Tau Or* 04 18 51.7036254480 +17 23 16.582694856   13.32 12.22 12.22 10.944 K7e 119 0
12 V* V830 Tau TT* 04 33 10.0300557048 +24 33 43.255480860   13.91 12.08 11.30   M0-1 201 1
13 V* AB Dor TT* 05 28 44.8712165880 -65 26 55.199147208 8.259 7.856 6.999 6.496 5.993 K0V 994 0
14 V* V1358 Ori BY* 06 19 08.0574987312 -03 26 20.361237864   8.52 7.95     G0V 107 0
15 V* LQ Hya BY* 09 32 25.5683895648 -11 11 04.692242760 9.316 8.761 7.891 7.288 6.815 K1Vp 439 0
16 * tau Boo Ro* 13 47 15.7381720026 +17 27 24.809555600 5.02 4.98 4.49 4.09 3.85 F7IV-V 953 1
17 V* EK Dra BY* 14 39 00.2104038120 +64 17 29.979649860   8.243 7.604     G1.5V 424 0
18 V* LQ Lup TT* 15 08 37.7353724976 -44 23 17.049423444 11.46 11.54 10.645 10.22 9.804 G8IVe 80 0
19 V* V889 Her BY* 18 34 20.1028767504 +18 41 24.234675864   8.00 7.449   6.720 G2V 132 0
20 V* BO Mic BY* 20 47 45.0056152368 -36 35 40.769832192   10.39 9.337   8.216 K3V(e) 188 0
21 * 61 Cyg A BY* 21 06 53.9395895022 +38 44 57.902349973 7.50 6.39 5.21 4.19 3.54 K5V 1005 0
22 BD+22 4409 BY* 21 31 01.7140062576 +23 20 07.374015564   10.240 9.245 8.6 7.965 K3Vke 168 0

To bookmark this query, right click on this link: simbad:objects in 2020A&A...643A..39C and select 'bookmark this link' or equivalent in the popup menu


2023.02.04-10:21:31

© Université de Strasbourg/CNRS

    • Contact