A search for p-modes and other variability in the binary system 85 Pegasi using MOST photometry

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Table 3:

Model parameters for several possible configurations of the 85 Peg system and flux ratios as measured through the MOST custom filter.
Star	M	R	$T_{\rm eff}$	$\Delta T^{i}$	Flux ratio	$A_{{\rm obs}}^{ii}$
	( $M_{\odot}$ )	( $R_{\odot}$ )	(K)	( $\sigma$ )	A/B	(mmag)
A	0.90	0.92	5460	3	14.1	4.5
Ba	0.55	0.48	4200	0
Bb	...	...	...	...
A	0.77	0.74	4845	15	1.5	0.48
Ba	0.72	0.68	4605	2
Bb	...	...	...	...
A	0.90	0.92	5460	3	15.2	4.9
Ba	0.52	0.46	4160	0.2
Bb	0.20	0.21	3650	...
A	0.77	0.74	4845	15	5.4	1.7
Ba	0.52	0.46	4160	0.2
Bb	0.20	0.21	3650	...

ⁱ The deviations in temperature to the observed value given in D'Antona et al. (2005) are given in terms of the standard deviation $\sigma$ .
ⁱⁱ $A_{{\rm obs}}$ indicates the observed amplitude scaled with the corresponding flux ratio. The expected amplitude due to backheating of star Bb on star Ba is about 0.1-0.2 mmag.

Source LaTeX | All tables | In the text

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