Table 2
Relevant stellar properties found in the literature search for the stars detected by LOFAR.
| Star name | Star type | Distance (pc) (1) | Spectral type | RHC (R⊙) | RCC (R⊙) | MHC (M⊙) | MCC (M⊙) |
|---|---|---|---|---|---|---|---|
| Sig CrB (TZ Crb) | RS CVn | 22.66 (2) | F9V+G0V (3) | 1.14 (3) | 1.1 (3) | 1.11 (3) | 1.08 (3) |
| BQ CVn | RS CVn | 178.6 | F5V+K0III-IV (4) | 1.3* | 7.4 (5) | – | – |
| FG UMa | RS CVn | 211.0 | G0-8V+G8IV (6) | 1.0* | 9.1 (7) | 1.50 (7) | 0.58 (7) |
| BF Lyn | BY Dra | 23.46 | K2V+dK (8) | 0.78 (9) | 0.78 (9) | 0.71 (10) | 0.71 (10) |
| DM UMa | RS CVn | 189.4 | K2III-IV (11) | 5.9 (12) | – | 1.2 (13) | – |
| EV Dra | RS CVn | 57.55 | G5V+K0V (14) | 0.96 (14) | 0.75 (14) | 0.98 (14) | 0.82 (14) |
| DG CVn (GJ3789) | RS CVn | 18.29 | M4Ve+M4Ve (15) | 0.4 (15) | 0.4 (15) | – | – |
| EZ Peg | RS CVn | 164.4 | G5III-IV+K0V (16) | 4.7* | 0.8* | – | – |
| BH CVn (HR 5110) | RS CVn | 46.15 | F2IV+K2IV (17) | 3.1 (17) | 3.27 (17) | 1.50 (18) | 0.42 (18) |
| WW Dra | RS CVn | 153.5 | G2IV-K0IV (19) | 2.3 (20) | 3.9 (20) | 1.36 (21) | 1.34 (21) |
| YY Gem | BY Dra | 15.1 | M1Ve+M1Ve (22) | 0.66 (22) | 0.58 (22) | 0.60 (23) | 0.59 (23) |
| II Peg | RS CVn | 39.36 | K2IV+M0-3V (24) | 3.4 (24) | 0.5* | 0.80 (24) | 0.40 (24) |
| BD+334462 | RS CVn | 217.8 | F7IV+K0III-IV (25) | 1.94 (25) | 5.3 (25) | 0.89+ (25) | 0.91+ (25) |
| FG Cam (HD 61396) | RS CVn | 312.8 (26) | K2III+K2-M0III (27) | 17.3 (27) | 14.4 (27) | 3.27 (27) | 0.38 (27) |
Notes. The stars are in order of processing date. RHC is the radius of the hot component (earlier spectral type), RCC is the radius of the cold component (later spectral type). MHC is the mass of the hot component and MCC is the massof the cold component. Radii denoted with an asterisk (*) are estimated by taking the known radius of a star with the same spectral type (Boyajian et al. 2012, 2013; Aurière et al. 2015). The masses of BD+334462 are Msin3(i) due to unknown inclination, and are therefore lower limits. All distance measures come from Gaia DR2, except for Sig CrB which is only available in the Hipparcos catalogue and FG Cam which is only available in Gaia DR1. DM UMa is not spectrally resolved, therefore we give the combined spectral type. The literature search was made significantly more convenient thanks to the catalogue ofChromospherically Active Binaries (Eker et al. 2008).
References. (1) (Brown et al. 2018); (2) (van Leeuwen 2007); (3) (Strassmeier & Rice 2003); (4) (Griffin 2009); (5) (Fekel 1997); (6) (Marino et al. 2002); (7) (Fekel et al. 2002); (8) (Montes et al. 2000); (9) (Montes et al. 1995); (10) (Tokovinin et al. 2006); (11) (O’Neal et al. 2004); (12) (Gunn et al. 1998); (13) (Crampton et al. 1979); (14) (Fekel et al. 2005); (15) (Osten et al. 2016); (16) (Montes et al. 1998); (17) (Eker & Doherty 1987); (18) (Little-Marenin et al. 1986); (19) (Frasca & Catalano 1994); (20) (Fernandez-Figueroa et al. 1994); (21) (Popper 1988); (22) (Qian et al. 2002); (23) (Torres & Ribas 2002); (24) (Berdyugina et al. 1998); (25) (Frasca et al. 2006); (26) (Brown et al. 2016); (27) (Griffin et al. 2006).
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