Curriculum Vitae

Not accounting for 1d perturbation understimates e, K 1 and hence f(M)Parameter A09 (All lines) C05 (HeII) SZ10 (HeII)P orb (days) 3.9061(1) 3.9060(2) 3.906 (fixed)To 2825.99(5) 1943.1(1) 5017.08(6)e 0.34(4) 0.35(4) 0.24(8)ω ( ○ ) 236.0(6) 226(3) 237(22)γ (km/s) 4.0(3) 17.2(7) 4(1)K 1 (km/s) 19.7(9) 25(1) 24(4)a 1 sin i (R ) 1.44(7) 1.8(1) 1.8(2)f(M) (M ) 0.0026(4) 0.0053(9) 0.0049(6)rms (km/s) 7.1 9.1 6.2A09: Aragona et al 2009C05: Casares et al. 2005SZ10: Szalai et al. 2010C10 (HeII) C10*C10: with 1d oscillationC10* : after subtracting 1d oscillation3.90597(9) 3.90608(8)2478.11(8) 2478.08(6)0.30(3) 0.35(3)215(6) 212(5)17.3(5) 17.3(5)23.1(9) 24.2(9)1.70(7) 1.75(7)0.0043(5) 0.0047(6)8.3 6.4Possibly due to non-radial oscillations, similar to Vela X-1, where 5km/s amplitude oscillations at ¼ Porb (i.e. 2.2d) are also detected(Quaintrell et al. 2003 A&A 401 313)It may also have an impact in VHE production because of the roleof stellar photons in IC scattering