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)
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)
A small group of X-ray binaries currently provides the best evidence for the existence of stellar-mass black holes. These objects are interacting binary systems where the X-rays arise from accretion of material onto a compact object (i.e. an object with a radius of less than a few hundred km). In some favourable cases, optical studies of the companion star(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 P sp = 1.552 ± 0.010 days and a semiamplitude of K 2 = 349 ± 12 km s −1. The optical mass function is f (M) = 6.86 ± 0.71 M ⊙ (1σ). We tentatively measure the(More)
We provide a comprehensive report on the X-ray and radio evolution of H1743–322 during its 2003 outburst. Our X-ray spectral and timing results (3–200 keV) are derived from 170 RXTE observations that span the complete 8-month outburst cycle. Our 6-frequency VLA light curves provide quite complete coverage of the entire outburst cycle at 4.860 GHz and 8.460(More)
An extensive grid of synthetic mid-and far-ultraviolet spectra for accretion disks in cata-clysmic variables has been presented by Wade and Hubeny (1998). In those models, the disk was assumed to be in steady-state, that is T eff (r) is specified completely by the mass M WD and radius R WD of the accreting white dwarf star and the mass transfer rate ˙ M(More)
We report on the X-ray spectral behavior of XTE J1550–564 during its 1998-99 outburst. XTE J1550–564 is an exceptionally bright X-ray nova and is also the third Galactic black hole candidate known to exhibit quasiperiodic X-ray oscillations above 50 Hz. Our study is based on 209 pointed observations using the PCA and HEXTE instruments onboard the Rossi(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 the detection of a planet whose orbit surrounds a pair of low-mass stars. Data from the Kepler spacecraft reveal transits of the planet across both stars, in addition to the mutual eclipses of the stars, giving precise constraints on the absolute dimensions of all three bodies. The planet is comparable to Saturn in mass and size and is on a nearly(More)