Orbital parameters of the microquasar LS I +61 303

By J. Casares, I. Ribas, J. Paredes, J. Martí, C. Allende Prieto. 2005

147 citations recorded by the source corpus.

New optical spectroscopy of the high-mass X-ray binary microquasar LS I +61 303 is presented. Eccentric orbital fits to our radial velocity measurements yield updated orbital parameters in good agreement with previous work. Our orbital solution indicates that the periastron passage occurs at radio phase 0.23 and the X-ray/radio outbursts are triggered 2.5-4 d after the compact star passage. The spectrum of the optical star is consistent with a B0 V spectral type and contributes ∼65 per cent of the total light, the remainder being the result of emission by a circumstellar disc. We also measure the projected rotational velocity to be v sin i ≃ 113 km s -1 .

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/6e71615f64f80d2bba5652ddf6e3e346df85a020

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In Astronomy and Astrophysics

1. P. Reig
2. W. Cui
3. G. Dubus
4. et al.
5. for the Belle collaboration
6. F. Krennrich
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In Nuclear and High Energy Physics

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2. W. Cui
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Citations in the corpus

• Gamma-ray binaries : pulsars in disguise? (2006, methodology): “Parameters as derived have higher, probably irreducible, systematics than the quoted (statistical) errors might suggest (e.g. Table 2 of Casares et al. 2005b).”
• VERITAS Observations of the γ-Ray Binary LS I +61 303 (2008, background): “Optical and radio observations of LS I +61 303 show that the compact object orbits the massive star every 26.496 days; the elliptical orbit is characterized by a semi-major axis of only a few stellar radii and an eccentricity of 0.72 ± 0.15 (Casares et al. 2005; Grundstrom et al. 2007).”
• Be/X-ray binaries (2011, background): “Radial velocity studies do not completely rule out this possibility (Casares et al. 2005a).”
• FERMI LAT OBSERVATIONS OF LS I +61°303: FIRST DETECTION OF AN ORBITAL MODULATION IN GeV GAMMA RAYS (2009, background): “The binary has an eccentric orbit (e=0.55-0.72) and the Be star radial velocity is consistent with a neutron star companion or, if the orbital inclination is≤ 25◦, with a≥ 3M⊙ black hole (Hutchings & Crampton 1981; Casares et al. 2005).”