Starspot Mapping with Adaptive Parallel Tempering. II. Application to TESS Data for M-dwarf Flare Stars AU Microscopii, YZ Canis Minoris, and EV Lacertae

被引：15

作者：

Ikuta, Kai ^{[1
]}

Namekata, Kosuke ^{[2
]}

Notsu, Yuta ^{[3
,4
,5
]}

Maehara, Hiroyuki ^{[1
,6
]}

Okamoto, Soshi ^{[7
,8
]}

Honda, Satoshi ^{[9
]}

Nogami, Daisaku ^{[7
]}

Shibata, Kazunari ^{[10
,11
]}

机构：

[1] Kyoto Univ, Astron Observ, Kitashirakawa Oiwake Cho,Sakyo, Kyoto 6068502, Japan

[2] NINS, Natl Astron Observ Japan, ALMA Project, Mitaka, Tokyo 1818588, Japan

[3] Univ Colorado, Lab Atmospher & Space Phys, 3665 Discovery Dr, Boulder, CO 80303 USA

[4] Natl Solar Observ, 3665 Discovery Dr, Boulder, CO 80303 USA

[5] Tokyo Inst Technol, Dept Earth & Planetary Sci, 2-12-1 Ookayama,Meguro, Tokyo 1528551, Japan

[6] NINS, Natl Astron Observ Japan, Okayama Branch Off, Subaru Telescope, Okayama 7190232, Japan

[7] Kyoto Univ, Dept Astron, Kitashirakawa Oiwake Cho,Sakyo, Kyoto 6068502, Japan

[8] Japan Meteorol Agcy, 1-3-4 Otemachi,Chiyoda, Tokyo 1008122, Japan

[9] Univ Hyogo, Nishi Harima Astron Observ, 407-2 Nishigaichi,Sayo Cho, Sayo, Hyogo 6795313, Japan

[10] Kyoto Univ, Kwasan Observ, 17 Ohmine Cho, Kyoto 6078471, Japan

[11] Doshisha Univ, Dept Environm Syst Sci, 1-3 Tataramiyakodani, Kyoto 6100394, Japan

来源：

ASTROPHYSICAL JOURNAL | 2023年 / 948卷 / 01期

关键词：

SOLAR-TYPE STARS; ANALYTIC SPOT MODELS; STELLAR FLARES; MAGNETIC ACTIVITY; UV CETI; STATISTICAL PROPERTIES; DIFFERENTIAL ROTATION; INFORMATION-CONTENT; SIGMA-GEMINORUM; DEBRIS DISK;

D O I：

10.3847/1538-4357/acbd36

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Starspots and stellar flares are indicators of stellar magnetic activity. The magnetic energy stored around spots is thought to be the origin of flares, but the connection is not completely understood. To investigate the relation between spot locations deduced from light curves and the occurrence of flares therein, we perform starspot modeling for the TESS light curves of three M-dwarf flare stars, AU Mic, YZ CMi, and EV Lac, using the code implemented in Paper I. The code enables us to deduce multiple stellar/spot parameters by the adaptive parallel tempering algorithm efficiently. We find that flare occurrence frequency is not necessarily correlated with the rotation phases of the light curve for each star. The result of starspot modeling shows that any spot is always visible to the line of sight in all phases, and we suggest that this can be one of the reasons why there is no or low correlation between rotation phases and flare frequency. In addition, the amplitude and shape of the light curve for AU Mic and YZ CMi have varied in two years between different TESS cycles. The result of starspot modeling suggests that this can be explained by the variations of spot size and latitude.

引用

页数：28