Physical Sciences and Mathematics Commons^™

Planetary Systems Around Close Binary Stars: The Case Of The Very Dusty, Sun-Like, Spectroscopic Binary Bd+20 307, Benjamin Zuckerman, Francis C. Fekel, Michael H. Williamson, Gregory W. Henry, Michael P. Muno

Information Systems and Engineering Management Research Publications

Field star BD+20 307 is the dustiest known main-sequence star, based on the fraction of its bolometric luminosity, ~4%, that is emitted at infrared wavelengths. The particles that carry this large infrared luminosity are unusually warm, comparable to the temperature of the zodiacal dust in the solar system, and their existence is likely to be a consequence of a fairly recent collision of large objects such as planets or planetary embryos. Thus, the age of BD+20 307 is potentially of interest in constraining the era of terrestrial planet formation. The present project was initiated with an attempt to derive this …

Multiwavelength Constraints On The Day–Night Circulation Patterns Of Hd 189733b, Heather Knutson, David Charbonneau, Nicolas B. Cowan, Jonathan J. Fortney, Adam P. Showman, Eric Agol, Gregory W. Henry, Mark E. Everett, Lori E. Allen

Information Systems and Engineering Management Research Publications

We present new Spitzer observations of the phase variation of the hot Jupiter HD 189733b in the MIPS 24 μm bandpass, spanning the same part of the planet's orbit as our previous observations in the IRAC 8 μm bandpass (Knutson et al. 2007). We find that the minimum hemisphere-averaged flux from the planet in this bandpass is 76% ± 3% of the maximum flux; this corresponds to minimum and maximum hemisphere-averaged brightness temperatures of 984 ± 48 K and 1220 ±  47 K, respectively. The planet reaches its maximum flux at an orbital phase of 0.396 ± 0.022, corresponding to …

Chemical Analysis Of Five Red Giants In The Globular Cluster M10 (Ngc 6254), Sharina Haynes, Geoffrey Burks, Christian I. Johnson, Catherine A. Pilachowski

Information Systems and Engineering Management Research Publications

We have determined Al, α, Fe-peak, and neutron capture elemental abundances for five red-giant branch (RGB) stars in the Galactic globular cluster M10. Abundances were determined using equivalent width analyses of moderate-resolution (R ∼ 15,000) spectra obtained with the Hydra multifiber positioner and bench spectrograph on the WIYN telescope. The data sample the upper RGB from the luminosity level near the horizontal branch to about 0.5 mag below the RGB tip. We find, in agreement with previous studies, that M10 is moderately metal-poor with [Fe/H] = -1.45 (σ = 0.04). All stars appear enhanced in Al with 〈[Al/Fe]〉 = +0.33 …

Infrared Spectroscopy Of Symbiotic Stars. Vi. Combined Orbits For Two S-Type Systems: V455 Scorpii And Ss 73-90, Francis C. Fekel, Kenneth H. Hinkle, Richard R. Joyce, Peter R. Wood, Ian D. Howarth

Information Systems and Engineering Management Research Publications

We have combined new infrared radial velocities and previously obtained spectropolarimetric observations to compute orbits of the M6 giants in two southern S-type symbiotic systems. The spectropolarimetric data enable the orbital inclinations of the systems to be determined, placing greater constraints on the properties of the components. V455 Sco has a circular orbit with a period of 1398 ± 6 days and an inclination of 94° ± 1°. The orbit of SS 73-90 has a period of 898 ± 5 days, a modest eccentricity of 0.16, and an inclination of 97° ± 7°. The center of mass velocity of each …

Orbits And Pulsations Of The Classical Ζ Aurigae Binaries, Joel A. Eaton, Gregory W. Henry, Andrew P. Odell

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We have derived new orbits for ζ Aur, 32 Cyg, and 31 Cyg with observations from the Tennessee State University (TSU) Automatic Spectroscopic Telescope, and used them to identify nonorbital velocities of the cool supergiant components of these systems. We measure periods in those deviations, identify unexpected long-period changes in the radial velocities, and place upper limits on the rotation of these stars. These radial-velocity variations are not obviously consistent with radial pulsation theory, given what we know about the masses and sizes of the components. Our concurrent photometry detected the nonradial pulsations driven by tides (ellipsoidal variation) in both …

The Chromospherically Active, Triple, Ellipsoidal, And Eclipsing Binary Hd 6286 = Be Piscium: A Laboratory For Binary Evolution, Klaus G. Strassmeier, János Bartus, Francis C. Fekel, Gregory W. Henry

Information Systems and Engineering Management Research Publications

Aims. We present a detailed analysis of the star HD 6286 = BE Psc from 16 years of spectroscopic observations and 18 seasons of photometric ones. The star is an evolved, chromospherically active, eclipsing binary, consisting of a K1 giant plus an F6 dwarf/subgiant in a circular orbit with a period of 35.671 days. A faint, close visual companion of spectral type ≈G0 makes the system triple. The orbital inclination of the eclipsing pair is 818.

Methods. We have obtained simultaneous solutions with our extensive set of radial velocities and light curves that include the star spot variability of …

Further Studies Of The Photometric Variability Of Bright Pulsating Red Giants, John R. Percy, Marina Mashintsova, Otilia Cristina Nasui, R. Palaniappan, R. Seneviratne, Gregory W. Henry

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Long-term photoelectric V photometry of 13 pulsating red giants (TV Psc, EG And, RZ Ari, η Gem, V614 Mon, RS Cnc, VY UMa, FS Com, SW Vir, R Lyr, EU Del, V1070 Cyg, and W Cyg) from a robotic telescope (APT) and from the photoelectric photometry program of the American Association of Variable Star Observers has been merged to form data sets that are significantly longer and denser than the subsets, and have been analyzed using Fourier and self-correlation techniques. Improved values of the pulsation periods, and especially of the enigmatic long secondary periods (LSPs), have been determined. Most of …

The Extremely Rapid Rotational Braking Of The Magnetic Helium-Strong Star Hd 37776, Zdeněk Mikulášek, Jiří Krtička, Gregory W. Henry, Juraj Zverko, Jozef Žižňovský, David A. Bohlender, Iosif I. Romanyuk, Jan Janík, Hrvoje Božić, D. Korčáková, Miloslav Zejda, Ivan Kh. Iliev, Petr Škoda, Miroslav Šlechta, Tomáš Gráf, Martin Netolický, Michal Ceniga

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Context. Light and spectrum variations of the magnetic chemically peculiar (mCP) stars are explained by the oblique rigid rotator model with a rotation period usually assumed to be stable on a long time scale. A few exceptions, such as CU Vir or 56 Ari, have been reported as displaying an increase in their rotation period. A possible increase in the period of light and spectrum variations has also been suggested from observations of the helium-strong mCP star HD 37776 (V901 Ori).

Aims. In this paper we attempt to confirm the possible period change of HD 37776 and discuss a possible …

Five New Transits Of The Super-Neptune Hd 149026b, Joshua N. Winn, Gregory W. Henry, Guillermo Torres, Matthew J. Holman

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We present new photometry of HD 149026 spanning five transits of its "super-Neptune" planet. In combination with previous data, we improve on the determination of the planet-to-star radius ratio: Rp/R⋆ = 0.0491+ 0.0018−0.0005. We find the planetary radius to be 0.71 ± 0.05 RJup, in accordance with previous theoretical models invoking a high metal abundance for the planet. The limiting error is the uncertainty in the stellar radius. Although we find agreement among four different ways of estimating the stellar radius, the uncertainty remains at 7%. We also present a refined transit ephemeris and a constraint on the orbital eccentricity …

Five Planets Orbiting 55 Cancri, Debra A. Fischer, Geoffrey W. Marcy, R. Paul Butler, Steve S. Vogt, Gregory Laughlin, Gregory W. Henry, David Abouav, Kathryn M. G. Peek, Jason T. Wright, John A. Johnson, Chris Mccarthy, Howard Isaacson

Information Systems and Engineering Management Research Publications

We report 18 years of Doppler shift measurements of a nearby star, 55 Cancri, that exhibits strong evidence for five orbiting planets. The four previously reported planets are strongly confirmed here. A fifth planet is presented, with an apparent orbital period of 260 days, placing it 0.78 AU from the star in the large empty zone between two other planets. The velocity wobble amplitude of 4.9 m s−1 implies a minimum planet mass Msin i = 45.7 M⊕. The orbital eccentricity is consistent with a circular orbit, but modest eccentricity solutions give similar χ2ν fits. All five planets reside in …

Masses, Luminosities, And Orbital Coplanarities Of The Μ Orionis Quadruple-Star System From Phases Differential Astrometry, Matthew W. Muterspaugh, Benjamin F. Lane, Francis C. Fekel, Maciej Konacki, Bernard F. Burke, Shrinivas R. Kulkarni, Mark M. Colavita, Michael Shao, Sloane J. Wiktorowicz

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μ Orionis was identified by spectroscopic studies as a quadruple-star system. Seventeen high-precision differential astrometry measurements of μ Ori have been collected by the Palomar High-precision Astrometric Search for Exoplanet Systems (PHASES). These show both the motion of the long-period binary orbit and short-period perturbations superimposed on that caused by each of the components in the long-period system being themselves binaries. The new measurements enable the orientations of the long-period binary and short-period subsystems to be determined. Recent theoretical work predicts the distribution of relative inclinations between inner and outer orbits of hierarchical systems to peak near 40 and 140 …

New Precision Orbits Of Bright Double-Lined Spectroscopic Binaries. Ii. Hr 2962, Hd 214686, And 16 Psc, Jocelyn Tomkin, Francis C. Fekel

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Radial velocities from the 2.1 m telescope at McDonald Observatory and the coudé feed telescope at Kitt Peak National Observatory are used to determine new spectroscopic orbits for the double-lined spectroscopic binaries HR 2962 (F5V), HD 214686 (F8IV), and 16 Psc (F6Vb vw). The new orbital dimensions (a1sin i and a2sin i) and minimum masses (m1sin3i and m2sin3i) have accuracies of 0.1–1%. In the case of HD 214686, which has components of nearly the same mass (m1/m2 = 1.0080 ± 0.0013), we confirm that the component labeled as the primary in previous spectroscopic studies of this system is the slightly …