X-ray variability of the triplet star system LTT1445 and evaporation history of the planets around its A component

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Volume 687 (July 2024)

A&A, 687 (2024) A237

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Table 8

X-ray properties for LTT 1445BC across observations.

Date	Observatory	Activity	Duration (ks)	f_X (10⁻¹³ erg cm⁻² s⁻¹)	log L_X	kT_peak (keV)	Ref.
2021-06-05	Chandra	Flare BC	5.2	20.2 ± 0.90	28.06 ± 0.02	0.38 ± 0.1^(*)	Brown 2022
2021-06-05	Chandra	Nonflare BC	23.4	7.3 ± 0.20	27.61 ± 0.01	0.76 ± 0.03	Brown 2022
2022 all	Chandra	Flare BC	6.20	${14.9}_{- 0.95}^{+ 0.93 (* )}$ $\[14.9_{-0.95}^{+0.93( *)}\]$	27.933 ± 0.027	0.81 ± 0.8	This work
2022 all	Chandra	Nonflare BC	47.8	${7.63}_{- 0.34}^{+ 0.34 (* )}$ $\[7.63_{-0.34}^{+0.34( *)}\]$	27.64 ± 0.019	0.43 ± 0.13	This work
2022-10-12	Chandra	C – Full	12.0	${10.86}_{- 1.09}^{+ 1.48}$ $\[10.86_{-1.09}^{+1.48}\]$	27.80 ± 0.05	0.33 ± 0.25	This work
2022-11-24	Chandra	B – Full	30.0	${5.88}_{- 0.59}^{+ 0.48}$ $\[5.88_{-0.59}^{+0.48}\]$	27.53 ± 0.04	0.82 ± 0.67	This work

Notes. ^(*)The lower temperature (kT₁) from the two temperature fit ^(**)Flux calculated for energy band 0.6–2.3 keV to match the eROSITA flux.

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