2002A&A...384.1038E


Query : 2002A&A...384.1038E

2002A&A...384.1038E - Astronomy and Astrophysics, volume 384, 1038-1049 (2002/3-4)

On the simultaneous optical and near-infrared variability of pre-main sequence stars.

EIROA C., OUDMAIJER R.D., DAVIES J.K., DE WINTER D., GARZON F., PALACIOS J., ALBERDI A., FERLET R., GRADY C.A., CAMERON A., DEEG H.J., HARRIS A.W., HORNE K., MERIN B., MIRANDA L.F., MONTESINOS B., MORA A., PENNY A., QUIRRENBACH A., RAUER H., SCHNEIDER J., SOLANO E., TSAPRAS Y. and WESSELIUS P.R.

Abstract (from CDS):

For a complete understanding of the physical processes causing the photometric variability of pre-main sequence systems, simultaneous optical and near-IR observations are required to disentangle the emission from the stars and that from their associated circumstellar disks. Data of this sort are extremely rare and little systematic work has been reported to date. The work presented in this paper is a systematic attempt in this direction. It presents an analysis of the simultaneous optical and near-IR photometric variability of 18 Herbig Ae/Be and T Tauri stars which were observed in October 98 by the EXPORT collaboration. The time difference between the UBVRI and JHK measurements is less than 1 hour in ≃50% of the data and the largest difference is around 2 hours in only ≃10% of the data. Twelve stars appear to show a correlation between the optical and near-IR variability trends, which suggests a common physical origin such as spots and/or variable extinction. The optical and near-IR variability is uncorrelated in the rest of the objects, which suggests it originates in distinctly different regions. In general, the optical variability qualitatively follows the predictions of starspots or variable extinction. As far as the near-IR is concerned, the simultaneity of the observations demonstrates that for most objects the flux is largely produced by their circumstellar disks and, consequently, in many cases the near-IR fluctuations must be attributed to structural variations of such disks producing variations of their thermal emission and/or scattered light. The observed near-IR changes of up to around 1 mag on timescales of 1-2 days provide interesting challenges for understanding the mechanisms generating such remarkable variabilities, an issue insufficiently investigated until now but one which deserves further theoretical and modeling efforts.

Abstract Copyright:

Journal keyword(s): stars: formation - stars: pre-main-sequence - stars: variables: general - stars: circumstellar matter - accretion, accretion disks

Simbad objects: 27

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Number of rows : 27
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 V* VX Cas Ae* 00 31 30.6818495040 +61 58 50.984946300 11.83 11.59 10.50 11.19 10.94 A0Vep 130 0
2 V* XY Per Ae* 03 49 36.3365862552 +38 58 55.548299928 12.12 10.14 9.58 9.54 8.40 A2II+B6 146 0
3 V* CW Tau Or* 04 14 17.0042670144 +28 10 57.766508508 13.92 13.64 12.36 12.86   K0Ve 337 0
4 V* RY Tau Or* 04 21 57.4092550080 +28 26 35.555316612 10.82 10.34 9.30 9.67 8.87 K1IV/Ve 675 1
5 V* DF Tau TT* 04 27 02.7932020080 +25 42 22.453341516 11.97 12.25 11.42 10.31 9.14 M3Ve 484 1
6 V* DK Tau A * 04 30 44.2408811328 +26 01 24.734232948           K5Ve 255 0
7 V* DK Tau Or* 04 30 44.243376 +26 01 24.65328 13.32 14.59 13.05 12.08   K7e+K7e 312 0
8 V* AA Tau Or* 04 34 55.4201902392 +24 28 53.033624580 13.14 13.34 12.20     K5Ve 687 0
9 V* DR Tau Or* 04 47 06.2151561264 +16 58 42.813872580 12.03 11.86 10.50 12.19   K5Ve 502 0
10 HD 31648 Ae* 04 58 46.2655706952 +29 50 36.987625680 7.84 7.78 7.62 7.76 7.43 A5Vep 464 0
11 V* UX Ori Ae* 05 04 29.9878898040 -03 47 14.286732072 10.25 10.93 8.70 9.62 9.43 A4IVe 352 1
12 V* V1366 Ori Ae* 05 16 00.4765181328 -09 48 35.393784012 10.19 10.16 9.84 9.77 9.63 B9.5V 185 0
13 HD 287841 Y*O 05 24 42.8032369656 +01 43 48.249234516 10.55 10.45 10.17 9.99 9.80 A8V 98 0
14 V* CO Ori Or* 05 27 38.3386648 +11 25 38.974625 12.96 12.33 10.30 10.33 9.63 F7Ve 162 0
15 V* HK Ori Ae* 05 31 28.049808 +12 09 10.30212 11.82 12.235 11.716 11.632 10.56 A2?e+G0?e 186 1
16 V* RY Ori Or* 05 32 09.9419233368 -02 49 46.770599784 12.62 12.76 10.80 10.82 10.34 F7 56 0
17 V* NV Ori Ae* 05 35 31.3686116448 -05 33 08.872027056 10.36 10.21 8.70 9.48 9.22 F6IIIe 97 0
18 V* T Ori Ae* 05 35 50.4482802768 -05 28 34.925254536 12.724 11.637 11.248 10.09 10.043 A3IVeb 243 0
19 V* CQ Tau Ae* 05 35 58.4666264136 +24 44 54.091450572 11.290 10.780 10.000   8.33 F5IVe 283 0
20 V* BF Ori Ae* 05 37 13.2623828280 -06 35 00.568242528 10.37 10.00 9.69 10.06 9.31 A7III 280 0
21 V* RR Tau Ae* 05 39 30.5115918672 +26 22 26.967444996 11.64 12.09 11.28 10.58 10.17 A0:IVe 222 0
22 V* V350 Ori Y*O 05 40 11.7638894112 -09 42 11.086012692 12.74 12.08 11.42 11.38 10.96 A7V 73 0
23 * bet Pic PM* 05 47 17.0876901 -51 03 59.441135 4.13 4.03 3.86 3.74 3.58 A6V 1796 1
24 V* VV Ser Ae* 18 28 47.8620017808 +00 08 39.923474964 12.99 12.63 11.80 11.01 10.24 A5Ve 242 0
25 V* WW Vul Ae* 19 25 58.7494120560 +21 12 31.333658616 11.46 10.99 10.25 10.38 10.12 A2IVe 221 0
26 V* PX Vul Or* 19 26 40.2532914312 +23 53 50.782579116 12.56 12.57 11.83 10.90 10.30 F3Ve 53 0
27 V* BM And Or* 23 37 38.4905191632 +48 24 11.762378244   12.40 12.40     K5Ve 82 1

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2022.09.28-01:07:40

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