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New Results on Stellar Flares Monitored with MAXI/GSC. Yohko Tsuboi , Kyohei Yamazaki, Akiko Uzawa, Takanori Matsumura (Chuo Univ.), Satoshi Nakahira (Aoyama Gakuin Univ.), Motoki Nakajima (Nihon Univ.), and the MAXI team. Stars detected with MAXI/GSC. Flare. Eta Carinae. T Tauri star.

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new results on stellar flares monitored with maxi gsc

New Results on Stellar Flares Monitored with MAXI/GSC

Yohko Tsuboi, Kyohei Yamazaki, Akiko Uzawa, Takanori Matsumura (Chuo Univ.), Satoshi Nakahira (Aoyama Gakuin Univ.), Motoki Nakajima (Nihon Univ.), and the MAXI team

stars detected with maxi gsc
Stars detected with MAXI/GSC

Flare

Eta Carinae

T Tauri star

Massive stellar

binary : 2

Low-mass star : 8

Single T Tauri star : 1

RS CVn binary : 7

theta Ori C

RS CVn stars

t tauri star twa 7
T Tauri star TWA-7
  • fast rotator
  • deep convection zone

V=19.2 km s-1

(cf. Vsun=0.6 km s-1)

TWA-7

x ray variability of twa 7
X-ray variability of TWA-7

Phase 2

Phase 0

Phase 1

td < 8 [ks]

spectrum of twa 7 flare
Spectrum of TWA-7 flare

Lx

= 1.2+0.3 ×1033

[erg s-1]

cf. Lx_sun

=1027[erg s-1]

-0.4

One of the

brightest

flare in those on T Tauri stars

log EM [cm-3] = 55.98

Lx [erg s-1] = 1.2 ×1033

(2-20keV , The error fixes kT. )

log EM [cm-3] = 55.98

Lx [erg s-1] = 1.2 ×1033

(2-20keV , The error fixes kT. )

log EM [cm-3] = 55.98

Lx [erg s-1] = 1.2 ×1033

(2-20keV , The error fixes kT. )

log EM [cm-3] = 55.98

Lx [erg s-1] = 1.2 ×1033

(2-20keV , The error fixes kT. )

log EM [cm-3] = 55.98

Lx [erg s-1] = 1.2 ×1033

(2-20keV , The error fixes kT. )

log EM [cm-3] = 55.98

Lx [erg s-1] = 1.2 ×1033

(2-20keV , The error fixes kT. )

+0.3

–0.4

rs cvn type stars
RS CVn type stars
  • close detached binaries
  • tidally locked
  • fast rotators

deep convection

zone

flares from rs cvn stars
Flares from RS CVn stars
  • 14 flares from 7 RS CVn binaries
  • 2 biggest flares in all the stellar flares

Lx = 5+4 ×1033 erg s-1

Lx = 4+1 ×1033 erg s-1

-2

-

II Peg

GT Mus

flare frequency
Flare frequency

Flares come

from specific stars

Then which component is special?

Interaction between each component is special?

Poisson distribution

(the expectation value is the same as that of the data)

spin velocity vs flares
Spin velocity vs flares

MAXI detected

MAXI non

detected

Spin velocity [km s-1]

Spin velocity [km s-1]

Probability that

two datasets

differ significantly

21%

44%

69% (not weighted)

97% (flare freq. weighted)

radius vs flares
Radius vs flares

MAXI detected

MAXI non

detected

Radius [solar radius]

Radius [solar radius]

Probability that

two datasets

differ significantly

96% (not weighted)

99.8% (flare freq. weighted)

10%

74%

binary parameters vs flares
Binary parameters vs flares

MAXI detected

MAXI non

detected

Separation [solar radius]

Orbital period [day]

51% (not weighted)

86% (flare freq. weighted)

11%

73%

Probability that

two datasets

differ significantly

summary
Summary
  • We increased the big flare samples (14 flares from 7 RS Cvns, 1 flare from 1 T Tauri star)
  • 2 biggest flares : II Peg : GT Mus: Lx = 4+-1 erg s-1
  • Hint for “Main big flare maker is subgiantcomponent”

 2, 3 years are needed to conclude

Lx = 5+4 erg s-1

-2

twa 7 rs cvn stars
TWA-7 RS CVn stars

Vcool=10-100 km s-1

V=19.2 km s-1