Jerome A. Orosz

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We report photometric and spectroscopic observations of the black hole binary GRO J1655-40 in complete quiescence. In contrast to the 1995 photometry, the light curves from 1996 are almost completely dominated by ellipsoidal modulations from the secondary star. Model fits to the light curves, which take into account the temperature profile of the accretion(More)
When an extrasolar planet passes in front of (transits) its star, its radius can be measured from the decrease in starlight and its orbital period from the time between transits. Multiple planets transiting the same star reveal much more: period ratios determine stability and dynamics, mutual gravitational interactions reflect planet masses and orbital(More)
Optical spectroscopic observations of the companion star (type G8IV to K4III) in the microquasar system XTE J1550-564 reveal a radial velocity curve with a best fitting spectroscopic period of Psp = 1:552 0:010 days and a semiamplitude of K2 = 349 12 km s−1. The optical mass function is f (M) = 6:86 0:71 M (1 ). We tentatively measure the rotational(More)
Spectroscopic observations of the soft X-ray transient 4U 1543-47 reveal a radial velocity curve with a period of P = 1.123 ± 0.008 days and a semi-amplitude of K2 = 124± 4 km s. The resulting mass function is f(M) = 0.22± 0.02M⊙. We classify the secondary star as A2V, in agreement with previous work, and measure Teff = 9000±500 K and E(B − V ) = 0.50 ±(More)
We report on the X-ray spectral behavior of XTE J1550[564 during its 1998È1999 outburst. XTE J1550[564 is an exceptionally bright X-ray nova and is also the third Galactic black hole candidate known to exhibit quasi-periodic X-ray oscillations above 50 Hz. Our study is based on 209 pointed observations using the PCA and HEXTE instruments on board the Rossi(More)
An extensive grid of synthetic midand far-ultraviolet spectra for accretion disks in cataclysmic variables has been presented by Wade and Hubeny (1998). In those models, the disk was assumed to be in steady-state, that is Teff(r) is specified completely by the mass MWD and radius RWD of the accreting white dwarf star and the mass transfer rate Ṁ which is(More)
In this letter we present several new three and four-planet solutions based on the most current available radial velocity data for HD160691 (μAra). These solutions are optimised using the Planetary Orbit Fitting Process (POFP) which is programmed and executed in MATLAB. POFP is based on a full integration of the system’s multiple-body Newtonian equations of(More)
We present the detection of five planets--Kepler-62b, c, d, e, and f--of size 1.31, 0.54, 1.95, 1.61 and 1.41 Earth radii (R⊕), orbiting a K2V star at periods of 5.7, 12.4, 18.2, 122.4, and 267.3 days, respectively. The outermost planets, Kepler-62e and -62f, are super-Earth-size (1.25 R⊕ < planet radius ≤ 2.0 R⊕) planets in the habitable zone of their host(More)
The Kepler spacecraft has been monitoring the light from 150,000 stars in its primary quest to detect transiting exoplanets. Here, we report on the detection of an eclipsing stellar hierarchical triple, identified in the Kepler photometry. KOI-126 [A, (B, C)], is composed of a low-mass binary [masses M(B) = 0.2413 ± 0.0030 solar mass (M(⊙)), M(C) = 0.2127 ±(More)
We report on the masses, sizes, and orbits of the planets orbiting 22 Kepler stars. There are 49 planet candidates around these stars, including 42 detected through transits and 7 revealed by precise Doppler measurements of the host stars. Based on an analysis of the Kepler brightness measurements, along with high-resolution imaging and spectroscopy,(More)