Table 3: The physical parameters of the two young eclipsing binaries RX J0529.4+0041 A and V1174 Ori as adopted from Covino et al. (2004) and Stassun et al. (2004), respectively. We use their temperature solutions but also determine a set of additional effective temperatures using other temperature scales (see Sect. 3.3).
RX J0529.4+0041 Aa RX J0529.4+0041 Ab

$M~[M_{\odot}]$ $1.27\pm0.01$ $0.93\pm0.01$

$R~[R_{\odot}]$ $1.44\pm0.05$ $1.35\pm0.05$

${\log}~g~[{\rm cgs}]$ $4.22\pm0.02$ $4.14\pm0.02$

$T_{\rm eff}~$ [K] $5200\pm150$ $4220\pm150$

spectral type K1 $\pm$ 1 K7-M0

V 1174 Ori A V 1174 Ori B

$M~[M_{\odot}]$ $1.009\pm0.015$ $0.731\pm0.008$

$R~[R_{\odot}]$ $1.339\pm0.015$ $1.065\pm0.011$

${\log}~g~[{\rm cgs}]$ $4.19\pm0.01$ $4.25\pm0.01$

$T_{\rm eff}~$ $4470\pm120$ $3615\pm100$

spectral type K4.5 $\pm$ 0.5 M 1.5

**Table 3:** The physical parameters of the two young eclipsing binaries RX J0529.4+0041 A and V1174 Ori as adopted from Covino et al. (2004) and Stassun et al. (2004), respectively. We use their temperature solutions but also determine a set of additional effective temperatures using other temperature scales (see Sect. 3.3).
	RX J0529.4+0041 Aa	RX J0529.4+0041 Ab
$M~[M_{\odot}]$	$1.27\pm0.01$	$0.93\pm0.01$
$R~[R_{\odot}]$	$1.44\pm0.05$	$1.35\pm0.05$
${\log}~g~[{\rm cgs}]$	$4.22\pm0.02$	$4.14\pm0.02$
$T_{\rm eff}~$ [K]	$5200\pm150$	$4220\pm150$
spectral type	K1 $\pm$ 1	K7-M0
	V 1174 Ori A	V 1174 Ori B
$M~[M_{\odot}]$	$1.009\pm0.015$	$0.731\pm0.008$
$R~[R_{\odot}]$	$1.339\pm0.015$	$1.065\pm0.011$
${\log}~g~[{\rm cgs}]$	$4.19\pm0.01$	$4.25\pm0.01$
$T_{\rm eff}~$	$4470\pm120$	$3615\pm100$
spectral type	K4.5 $\pm$ 0.5	M 1.5

Source LaTeX | All tables | In the text

	1 Introduction
	2 A new method - extending the approach of White et al. (1999)
	3 Application to known eclipsing binaries
	4 Summary and conclusions
	References
	Online Material
	Appendix A: Derivation of intrinsic scale errors
	Appendix B: Conversion tables