2011A&A...527A..96K


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.08CEST02:26:59

2011A&A...527A..96K - Astronomy and Astrophysics, volume 527A, 96-96 (2011/3-1)

Hunting for millimeter flares from magnetic reconnection in pre-main sequence spectroscopic binaries.

KOSPAL A., SALTER D.M., HOGERHEIJDE M.R., MOOR A. and BLAKE G.A.

Abstract (from CDS):

Recent observations of the low-mass pre-main sequence (PMS), eccentric spectroscopic binaries DQTau and V773TauA reveal that their millimeter spectrum is occasionally dominated by flares from non-thermal emission processes. The transient activity is believed to be synchrotron in nature, resulting from powerful magnetic reconnection events when the separate magnetic structures of the binary components are briefly capable of interacting and forced to reorganize, typically near periastron. We conducted the first systematic study of the millimeter variability toward a sample of 12 PMS spectroscopic binaries with the aim to characterize the proliferation of flares amongst sources likely to experience similar interbinary reconnection events. The source sample consists entirely of short-period, close-separation binaries that possess either a high orbital eccentricity (e>0.1) or a circular orbit (e≃0). Using the MAMBO2 array on the IRAM 30m telescope, we carried out continuous monitoring at 1.25mm (240GHz) over a 4-night period during which all of the high-eccentricity binaries approached periastron. We also obtained simultaneous optical VRI measurements, since a strong link is often observed between stellar reconnection events (traced via X-rays) and optical brightenings. UZ Tau E is the only source to be detected at millimeter wavelengths, and it exhibited significant variation (F1.25mm=87-179mJy); it is also the only source to undergo strong simultaneous optical variability (ΔR≃0.9mag). The binary possesses the largest orbital eccentricity in the current sample, a predicted factor in star-star magnetic interaction events. With orbital parameters and variable accretion activity similar to DQ Tau, the millimeter behavior of UZ Tau E draws many parallels to the DQ Tau model for colliding magnetospheres. However, on the basis of our observations alone, we cannot determine whether the variability is repetitive, or if it could also be due to variable free-free emission in an ionized wind. UZ Tau E brings the number of known millimeter-varying PMS sources to 3 out of a total of 14 monitored binaries now in the literature. Important factors in the non-detection of the rest of our targets are the coarse time-sampling and limited millimeter sensitivity of our survey. We recommend that future studies concentrate on close-by targets, and obtain millimeter and optical data points with better temporal resolution.

Abstract Copyright:

Journal keyword(s): stars: pre-main sequence - binaries: spectroscopic - stars: variables: general - radio continuum: stars - stars: flare - stars: individual: UZ Tau E

Simbad objects: 36

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Number of rows : 36

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 UCAC2 26810801 * 03 50 18.5685032431 -13 54 48.875491800       14.54   ~ 1 0
2 V* LO Eri RS* 03 50 30.8228458244 -13 55 29.757023428   11.65 10.759   9.816 K0-K1+K1-K2 21 0
3 HD 283447 Or* 04 14 12.9232870093 +28 12 12.378540314 13.17 12.07 10.68 9.45 8.67 K3Ve 380 0
4 GSC 01270-00357 * 04 32 03.5948717706 +18 06 03.705949742   16.9       ~ 4 0
5 V* V826 Tau TT* 04 32 15.8394065935 +18 01 38.751126168   13.51 12.074   10.312 K7.0 164 0
6 [ABG2007] 1457 * 04 32 30.2309385344 +25 52 41.399665772 18.05 16.4   13.8   ~ 3 0
7 V* UZ Tau B TT* 04 32 42.82968 +25 52 31.4148   14.07 12.72 13.35   M1/3Ve 136 0
8 V* UZ Tau ** 04 32 43.02168 +25 52 30.9036           M4Ve+M1/3Ve 285 0
9 V* UZ Tau A TT* 04 32 43.0744163742 +25 52 31.022242441       13.15   M2.0e+M3.0e 88 0
10 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 3478 0
11 V* DQ Tau Or* 04 46 53.0577037389 +17 00 00.135310040 14.56 13.67 12.00 13.21   M1Ve 286 0
12 TYC 101-1679-1 * 05 29 17.3789679625 +00 42 58.304989776   12.07 11.76 11.44   ~ 2 0
13 V* V1642 Ori A * 05 29 20.6218092175 +00 41 27.941912748           K1V 14 0
14 V* V1642 Ori TT* 05 29 20.633592 +00 41 27.99600   13.31 12.31 12.03   K2 45 0
15 V* V1642 Ori B * 05 29 20.7034682359 +00 41 28.527876492           K7-M0 2 0
16 UCAC2 30137855 * 05 30 31.4962345218 -04 34 53.687029093       11.81   ~ 1 0
17 V* V1878 Ori Or* 05 30 42.6347868035 -04 35 01.899769035   12.60 11.521   10.221 K3e 25 0
18 Brun 334 pr* 05 34 39.7639432774 -05 24 25.589725695 14.065 12.535 11.606   9.794 K3V+K5V 75 0
19 Brun 335 Em* 05 34 39.8796240506 -05 26 41.981423823   13.56 12.57     K0IV 41 0
20 NAME Orion Nebula Cluster OpC 05 35.0 -05 29           ~ 1977 1
21 V* V2212 Ori Al* 05 35 11.1412127665 -05 36 51.210193000 18.461 16.619 15.379   12.444 M2 49 0
22 MLLA 761 TT* 05 35 11.8040700 -05 21 49.266135           K5V 49 0
23 Brun 548 *iN 05 35 12.3594579123 -05 36 40.328754135 16.181 14.921 14.187   12.886 K2.7 20 0
24 NAME Orion-KL SFR 05 35 14.16 -05 22 21.5           ~ 2001 1
25 UCAC3 168-22738 * 05 37 09.2288963484 -06 06 44.518510884       13.16 12.23 ~ 1 0
26 V* V1814 Ori Or* 05 37 09.5213309361 -06 06 16.310368196   11.62 10.622 10.24 9.578 K0IV/V 40 0
27 V* V2758 Ori Or* 05 41 23.9429612738 -03 24 46.017364551   12.49 11.37     K1 15 0
28 UCAC2 30640176 * 05 41 28.6306072232 -03 26 58.252440157       12.24 11.55 ~ 1 0
29 V* GG Ori Al* 05 43 10.2225202776 -00 41 14.794297965   10.92       A2 66 0
30 HD 290841 PM* 05 43 15.5357707244 -00 36 54.576596333   11.5 10.7     K0 4 0
31 2MASS J06405783+0956299 TT* 06 40 57.8280574454 +09 56 29.880626134 15.174 14.79 13.752 13.196 12.688 ~ 19 0
32 NGC 2264 134 TT* 06 40 59.3436202135 +09 55 20.166584605 13.918 13.22 12.38 11.908 11.438 G5V 48 0
33 NGC 2266 OpC 06 43 20 +26 59.1     9.5     ~ 52 0
34 NAME CrA Dark Cloud MoC 19 01 51 -36 58.9           ~ 394 0
35 UCAC3 320-71607 * 21 40 28.0560769247 +69 40 32.725415956       12.32   ~ 1 0
36 V* EK Cep Al* 21 41 21.5039950844 +69 41 34.108387051   7.95 7.89     A0V 198 0

    Equat.    Gal    SGal    Ecl

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2020.07.08-02:26:59

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