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


Query : 2011A&A...527A..96K

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 - 2023
#notes
1 UCAC2 26810801 * 03 50 18.5685781656 -13 54 48.874011804       14.54   ~ 1 0
2 V* LO Eri RS* 03 50 30.8226917856 -13 55 29.757472356   11.65 10.759   9.816 K0-K1+K1-K2 23 0
3 HD 283447 Or* 04 14 12.9261150912 +28 12 12.359055168 13.17 12.07 10.68 9.45 8.67 K3Ve 410 0
4 GSC 01270-00357 * 04 32 03.5950153776 +18 06 03.704550948   16.9       ~ 4 0
5 V* V826 Tau TT* 04 32 15.8393134800 +18 01 38.750623752   13.51 12.074   10.312 K7.0 175 0
6 2MASS J04323023+2552413 * 04 32 30.2311152576 +25 52 41.401588080 18.05 16.4   13.8   ~ 5 0
7 V* UZ Tau Y*O 04 32 42.81 +25 52 31.3           M4Ve+M1/3Ve 309 0
8 V* UZ Tau B TT* 04 32 42.8118779016 +25 52 31.198173600   14.07 12.72 13.35   M1/3Ve 149 0
9 V* UZ Tau A TT* 04 32 43.0720716552 +25 52 31.013712120       13.15   M2.0e+M3.0e 124 0
10 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 4263 0
11 V* DQ Tau Or* 04 46 53.0575226016 +17 00 00.136127304 14.56 13.67 12.00 13.21   M1Ve 332 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 Y*? 05 29 20.6215098192 +00 41 27.948799752           K1V 15 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 20.7018230760 +00 41 28.552644384           K7-M0 2 0
16 UCAC2 30137855 * 05 30 31.4962256280 -04 34 53.686907400       11.81   ~ 1 0
17 V* V1878 Ori Or* 05 30 42.6347292144 -04 35 01.901663412   12.60 11.521   10.221 K3e 30 0
18 Brun 334 Y*O 05 34 39.7638260448 -05 24 25.590693312 14.065 12.535 11.606   9.794 K3V+K5V 83 0
19 Brun 335 Y*O 05 34 39.8798513832 -05 26 41.979432984   13.56 12.57     K0IV 47 0
20 NAME Orion Nebula Cluster OpC 05 35.0 -05 29           ~ 2270 0
21 V* V2212 Ori Y*O 05 35 11.1413470656 -05 36 51.212579400 18.461 16.619 15.379   12.444 M2 58 0
22 COUP 450 TT* 05 35 11.8040700 -05 21 49.266135           K5V 58 0
23 Brun 548 * 05 35 12.3594774504 -05 36 40.327530444 16.181 14.921 14.187   12.886 K2.7 22 0
24 NAME Orion-KL SFR 05 35 14.16 -05 22 21.5           ~ 2252 1
25 UCAC3 168-22738 * 05 37 09.2289882336 -06 06 44.519246820       13.16 12.23 ~ 1 0
26 V* V1814 Ori Or* 05 37 09.5211327120 -06 06 16.309879272   11.62 10.622 10.24 9.578 K0IV/V 42 0
27 V* V2758 Ori Or* 05 41 23.9428581864 -03 24 46.016418492   12.49 11.37     K1 17 0
28 UCAC2 30640176 * 05 41 28.6305322488 -03 26 58.249402044       12.24 11.55 ~ 1 0
29 V* GG Ori EB* 05 43 10.2226873248 -00 41 14.798359644   10.92       A2 76 0
30 HD 290841 SB* 05 43 15.5383690848 -00 36 54.657637632   11.5 10.7     K0 7 0
31 NGC 2264 389 TT* 06 40 57.8280675864 +09 56 29.881747500 15.174 14.79 13.752 13.196 12.688 ~ 28 0
32 NGC 2264 134 TT* 06 40 59.3436338472 +09 55 20.165321712 13.918 13.22 12.38 11.908 11.47 G5V 56 0
33 NGC 2266 OpC 06 43 19.7 +26 58 34     9.5     ~ 74 0
34 NAME Corona Australis Cloud MoC 19 01 51 -36 58.9           ~ 476 0
35 UCAC3 320-71607 * 21 40 28.0557597312 +69 40 32.726381880       12.32   ~ 1 0
36 V* EK Cep SB* 21 41 21.5042268336 +69 41 34.112933916   7.95 7.89     A0V 211 0

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2023.10.05-05:10:59

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