The Eclipsing Double-Lined Spectroscopic Binary System V505 Persei.

Abstract

The recently-discovered eclipsing double-lined spectroscopic binary V505 Persei (SAO 23229) consists of two nearly identical F5 main sequence stars in a 4.2 day orbit. We have obtained both spectroscopic and photometric observations of the binary that densely sample the complete cycle of radial velocity and light variations. These observations have been used to determine the elements of the orbit, to determine individual masses of the stars in the system to a precision of better than 1%, and to estimate an age for the system. The derived properties agree well with current stellar structure models and provide fundamental data for tests of stellar evolution theory.

Detached double-lined eclipsing binaries as critical tests of stellar evolution

“…However in our sample this is unlikely to be the case: (1) We have computed the Roche radii of the components and checked that they were much larger than the stellar radii (Lastennet 1998, from the formula of Eggleton 1983), and (2) most of the systems are still between the ZAMS and the TAMS, and their radii should not have evolved significantly. The hypothesis of independent evolution without phases of 5 RT And (Popper 1994), AD Boo (Lacy 1997b), SW CMa (Lacy 1997c), AH Cep (Holmgren et al 1990), CG Cyg (Popper 1994), Y Cyg (Simon et al 1994), CM Dra (Viti et al 1997), AG Per (Giménez & Clausen 1994), V505 Per (Marschall et al 1997), V3903 Sgr (Vaz et al 1993;Vaz et al 1997), V526 Sgr and YY Sgr (Lacy 1997a).…”

“…Although in some special cases strong constraints can be placed on the evolution of the system (e.g. Daems, Waelkens & (Lacy 1997c), AH Cep (Holmgren et al 1990), CG Cyg (Popper 1994), Y Cyg (Simon, Sturm & Fielder 1994), CM Dra (Viti et al 1997), AG Per (Giménez & Clausen 1994), V505 Per (Marschall et al 1997), V3903 Sgr (Vaz et al 1993, Vaz et al 1997, V526 Sgr and YY Sgr (Lacy 1997a).…”

Evaluating GAIA performances on eclipsing binaries

“…The photometric data were plotted and the mean of the maxima used to normalize the light of the system. The initial epoch and period were taken from the Hipparcos solution (listed in the Hipparcos Catalogue) or from Marschall et al (1997) for V505 Per, the temperature of the hotter star from the spectral classification, the initial temperature of the cooler star from the ratio of the depths of the minima, initial potentials set arbitrarily so that the stars did not exceed their critical surfaces (in modeling contact and over-contact systems, this procedure is changed, of course). Initially, all runs were carried out with linear limb-darkening and single-pass reflection treatment.…”

Evaluating the Gaia Contribution to the Field of Eclipsing Binaries with Ground-Based Spectroscopy and Hipparcos Photometry

“…This is a fantastic number compared to 100 systems studied at similar accuracy by ground-based observations so far. Moreover most of the Gaia binaries will be of G-K spectral type (Zwitter & Henden 248 P. G. Niarchos et al 20.86(10) 0.65(8) 0.98(10) 1.18(12) 0.99(14) 0.33(10) BS Dra 21.29(8) 1.28(9) 1.46(2) 1.40(7) 3.61(4) 3.34(18) GK Dra 21.46(7) 1.81(7) 2.43(4) 2.83(5) 13.26(15) 15.84(18) HP Dra 21.10(2) 1.10(3) 1.17(3) 0.89(9) 1.57(5) 1.16(16) UV Leo 21.21(9) 1.11(10) 0.97(2) 1.22(4) 1.17(4) 1.43(7) UW LMi 21.06(2) 1.04(2) 1.23(5) 1.21(6) 2.39(16) 2.31(7) CN Lyn 21.04(2) 1.04(2) 1.80 21 2(1): ground-based observations (Marschall et al 1997), 2: Gaia (expected) obs. (Munari et al 2001, Marrese et al 2004, Milone et al 2005 RZ Dra (1) 1.40(4) 0.62(3) 1.62(1) 1.12(1) 10.1(4) 1.01(6) RZ Dra 21.42(5) 0.59(4) 1.55(1) 1.11(1) 9.60(47) 0.86(5) % difference 1.4 4.8 4.3 0.9 5 15 V1010 Oph (1) 1.87(12) 0.90(5) 2.08(6) 1.48(8) 10.7(7) 3.47(35) V1010 Oph (2) 1.88(14) 0.89(7) 2.08(1) 1.46(1) 11.7(8) 3.07(8) % difference 0.5 1.1 0 1.4 9.3 12 AB And (1) 1.01(2) 0.56(1) 1.04(4) 0.80(5) 0.87(7) 0.46(5) AB And (2) 1.00(9) 0.55(5) 1.06(4) 0.83(5) 0.91(7) 0.45(5) % difference 1.0 1.8 1.9 3.7 4.6 2.2 CrA (1) 1.75(4) 0.21(2) 2.20(3) 0.80(1) 11.1(1) 1.08(1) CrA (2) 1.69(7) 0.22(5) 2.12(12) 0.80(4) 10.3(20) 1.07(14) % difference 3.4 4.8 3.6 1.2 7.2 0.9 YY CrB (1) 1.41(9) 0.34(2) 1.40(7) 0.77(10) 2.46(26) 0.81(20) YY CrB (2) 1.37(16) 0.33(4) 1.36(7) 0.74(10) 2.33(25) 0.74(20) % difference 2.8 2.9 2.9 3.9 5.3 8.6 XY Leo (1) 0.82(4) 0.41(2) 0.87(1) 0.64(2) 0.38(2) 0.14(1) XY Leo (2) 0.83(21) 0.41(10) 0.86(1) 0.62(2) 0.37(2) 0.17(1) % difference 1.2 0.7 1.1 3.1 2.6 21.4 XZ Leo (1) 1.83(5) 0.64(2) 1.71(2) 1.07(3) 7.29(29) 2.56(16) XZ Leo (2) 1.82(13) 0.63(6) 1.71(2) 1.07(3) 7.26(29) 2.69(19) % difference 0.5 1.6 0.2 0.2 0.4 5.1 V566 Oph (1) 1.40(3) 0.33(1) 1.47(1) 0.79(1) 4.57(4) 1.26(1) V566 Oph (2) 1.54(11) 0.36(4) 1.518(3) 0.819(4) 4.99(24) 1.26(2) % difference 10 9.1 3.5 3.7 9.2 0.8 V839 Oph (1) 1.62(4) 0.49(1) 1.53(6) 0.93(8) 3.12(26) 1.32(23) V839 Oph (2) 1.61(17) 0.49(5) 1.52(6) 0.92(8) 3.10(26) 1.22(21) % difference 0.6 0.8 0.7 1.1 0.6 7.6 AH Vir (1) 1.45(13) 0.44(4) 1.36(1) 0.77(1) 2.45(8) 0.71(2) AH Vir 21.33(20) 0.40(6) 1.44(1) 0.88(1) 2.76(9) 0.91(3) % difference 8.3 9.1 5.9 14.3 12.7 28.2…”