Research output: Contribution to journal › Article › peer-review
Unusual Photometric Activity of the Weak-line T Tauti Star V715 Per. / Grinin, V. P.; Barsunova, O. Yu; Sergeev, S. G.; Arkharov, A. A.; Shugarov, S. Yu; Semenov, A. O.; Efimova, N. V.
In: Astronomy Reports, Vol. 62, No. 10, 01.10.2018, p. 677-688.Research output: Contribution to journal › Article › peer-review
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TY - JOUR
T1 - Unusual Photometric Activity of the Weak-line T Tauti Star V715 Per
AU - Grinin, V. P.
AU - Barsunova, O. Yu
AU - Sergeev, S. G.
AU - Arkharov, A. A.
AU - Shugarov, S. Yu
AU - Semenov, A. O.
AU - Efimova, N. V.
N1 - Publisher Copyright: © 2018, Pleiades Publishing, Ltd.
PY - 2018/10/1
Y1 - 2018/10/1
N2 - The results of many-year photometric observations of the weak-line T Tauri star V715 Per in the optical (V RI) and infrared (JHK) photometric bands are presented. The period of the star’s lowamplitude brightness variations in the V RI bands detected earlier, 5.23d, is confirmed. This period persists during the entire 14-year time interval of the observations, but its amplitude varies with time. The same period was found in the variations of JHK infrared fluxes, with the brightness variations in the two ranges being almost synchronous. The most probable origin of these variations is periodic eclipses of the star by its own disk, perturbed by its interaction with the magnetosphere (AA Tau-type variations). In addition to the periodic brightness variations, the star also displayed sporadic Algol-like minima characteristic of UX Ori stars during several years (2005–2011). The amplitude of these variations increasedmonotonically, reaching approximately 1m in the V band by the end of 2010, after which the deep fadings ended. During this entire time interval, the amplitude of the periodic variations was observed to decrease. After 2011, the periodic component began to become stronger again. These changes of the photometric activity of V715 Per can be explained by an increasing rate of gas accretion onto the star, decreasing the radius of warped regions of the disk and leading to accompanying Algol-like fadings. This model assumes a low inclination of the circumstellar disk in V715 Per to the line of sight.
AB - The results of many-year photometric observations of the weak-line T Tauri star V715 Per in the optical (V RI) and infrared (JHK) photometric bands are presented. The period of the star’s lowamplitude brightness variations in the V RI bands detected earlier, 5.23d, is confirmed. This period persists during the entire 14-year time interval of the observations, but its amplitude varies with time. The same period was found in the variations of JHK infrared fluxes, with the brightness variations in the two ranges being almost synchronous. The most probable origin of these variations is periodic eclipses of the star by its own disk, perturbed by its interaction with the magnetosphere (AA Tau-type variations). In addition to the periodic brightness variations, the star also displayed sporadic Algol-like minima characteristic of UX Ori stars during several years (2005–2011). The amplitude of these variations increasedmonotonically, reaching approximately 1m in the V band by the end of 2010, after which the deep fadings ended. During this entire time interval, the amplitude of the periodic variations was observed to decrease. After 2011, the periodic component began to become stronger again. These changes of the photometric activity of V715 Per can be explained by an increasing rate of gas accretion onto the star, decreasing the radius of warped regions of the disk and leading to accompanying Algol-like fadings. This model assumes a low inclination of the circumstellar disk in V715 Per to the line of sight.
UR - http://www.scopus.com/inward/record.url?scp=85053926911&partnerID=8YFLogxK
U2 - 10.1134/S1063772918100049
DO - 10.1134/S1063772918100049
M3 - Article
AN - SCOPUS:85053926911
VL - 62
SP - 677
EP - 688
JO - Astronomy Reports
JF - Astronomy Reports
SN - 1063-7729
IS - 10
ER -
ID: 87424346