The Ninth Catalogue of Spectroscopic Binary Orbits (http://sb9.astro.ulb.ac.be) continues the series compilations spectroscopic orbits carried out over past 35 years by Batten and collaborators. As 2004 May 1st, new holds for 2386 systems. Some essential differences between this catalogue its predecessors are outlined three straightforward applications presented: (1) completeness assessment: period distribution SB1s SB2s; (2) shortest periods across H-R diagram; (3) period-eccentricity relation.

ABSTRACT Spectroscopic orbital elements are determined for 15 stars with periods from 8 to 6528 days six orbits computed the first time. Improved astrometric two and one new orbit is derived. Visual were previously four stars, members of multiple systems, five have Hipparcos “G” designations or been resolved by speckle interferometry. For nine binaries previous spectroscopic orbits, we determine improved comparable elements. HD 28271 200790, our results support conclusions authors that large...

A calibration based on the results of Gray has been used to determine projected rotational velocities for 133 bright stars with spectral types F, G, or K, most which appear in {The Bright Star Catalogue}. The vast majority have {v} sin {i} ≤q 10 km s-1 and, thus, are slow rotators. With new calibration, determined a sample 111 late-type stars, chromospherically active. Some had their measured first time.

We obtained spectroscopic and photometric observations of the γ Doradus variable HR 6844 (=V2502 Ophiuchi). Radial velocities show that this star is a single-lined binary with period 4.4852 days. The primary an F1 V star, while secondary likely M dwarf. Velocity residuals to circular orbit have 1.3071 days amplitude ∼3 km s-1. Three periods light variation were detected, 1.30702, 1.4350, 0.62286 first essentially identical found in radial has largest amplitude, peak-to-peak value 0.067 mag...

First results are reported for a program of monitoring symbiotic-star velocities in the 1.6 μm region with infrared-array technology. Infrared radial have been used to determine single-lined spectroscopic orbits six well-known symbiotic stars, EG And, T CrB, CI Cyg, BX Mon, RS Oph, and AG Peg. The new general agreement previous derived from optical velocities. From combined infrared improved orbital elements systems determined. Each periods has determined solely radial-velocity data. With...

view Abstract Citations (224) References (59) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS Chromospheric CA II H and K alpha Emission in Single Binary Stars of Spectra Types F6--M2 Strassmeier, Klaus G. ; Fekel, Francis C. Bopp, Bernard W. Dempsey, Robert Henry, Gregory New observations the Ca H-epsilon region and/or Balmer H-alpha line are presented for 100 mostly very active stars but also weak or inactive with suspected activity. Correlations between...

We have completed an automated photometric survey of 66 potential or known chromospherically active late-type stars with the 0.4 m Vanderbilt/Tennessee State robotic telescope. The precision observations from this telescope matches that predicted photon and scintillation noise alone represents a significant improvement in previous surveys stars. Light variability has been detected its period determined for 47 stars, 41 which are newly discovered variables. primary mechanism is rotational...

We present the results of an analysis time-series photometry, Ca II H and K spectrophotometry, high-dispersion visible spectra nine nearby Sun-like stars recently identified as having planets. For six whose presumed planets have orbital periods less than 4 months (τ Boo, 51 Peg, υ And, ρ1 Cnc, ρ CrB, 70 Vir), sine-curve fits to photometric data show no variations with semiamplitude greater 1 or 2 parts in 104. Photometric 47 UMa are similarly small, although our this star slightly affected...

view Abstract Citations (141) References (94) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS Lithium and Rapid Rotation in Chromospherically Active Single Giants Fekel, Francis C. ; Balachandran, Suchitra The rotational velocities presently obtained via spectroscopic observations of a group moderately rapidly rotating, chomospherically active single giants indicate that Gray's (1989) rotostat hypothesis requires modification. Their rapid rotation appears to...

Planets have been reported orbiting the Sun-like stars ρ1 Cnc, τ Boo, and υ And based on low-amplitude radial velocity variations. We derived information first two from analysis of spectra, as well parallel records high-precision Strömgren b y photometry Ca II H + K fluxes. In case upper limit (peak to peak) nondetection photometric variability at orbital period is Δy ~ 0.0004 mag. The possibility a planetary transit cannot be ruled out completely data. Variations fluxes suggest rotational...

view Abstract Citations (248) References (112) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS A Survey of Chromospherically Active Stars Fekel, F. C. ; Moffett, T. J. Henry, G. W. Photometric and/or spectroscopic observations have been obtained 52 late-type stars which are suspected or known to be chromospherically active. Although not all types were for each star, these include all-sky BVRI Johnson photometry, ultraviolet spectrograms, low-dispersion...

We have discovered the first example of a star pulsating intrinsically with both γ Doradus and δ Scuti frequencies. The star, HD 8801, is an Am metallic-line that appears to be single. Since vast majority stars are members binary systems periods less than 1000 days also do not pulsate, 8801 possesses very unusual, if unique, combination physical properties. Our photometry, acquired automatic telescope at Fairborn Observatory, resolves six independent pulsation between 0.048 0.404 days. two...

We have used three automatic photoelectric telescopes to obtain photometric observations of 187 G, K, and (a few) M0 field giants. find low-amplitude variability on timescales days weeks both sides the coronal dividing line (CDL) in a total 81 or 43% About one-third variables amplitudes greater than 0.01 mag V. In our sample percentage variable giants is minimum for late-G spectral classes increases earlier later classes; all K5 are variable. also obtained high-resolution, red wavelength...

Abstract A single-lined spectroscopic orbit for the M giant in X-ray binary IGR J16194−2810 is determined from a time series of optical spectra. The orbital period 192.5 days twice that photometric period, confirming system an ellipsoidal variable. identified as first ascent approaching red tip. primary neutron star (NS) with its companion filling Roche lobe, verifying classification low-mass (LMXB). Stellar C, N, O, and Fe abundances are derived O values typical field [Fe/H] = −0.14. does...

We present new high-dispersion spectroscopic and precise photometric observations to identify 11 γ Doradus variables. Seven of these stars appear be single, three are primaries single-lined binaries, one has two distant visual companions; none double-lined or close binaries. Several the show line-profile low-amplitude radial velocity variability indicative pulsation. All photometrically variable with amplitudes between 8 93 mmag in Johnson B periods 0.398 2.454 days. One star is...

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

We have determined improved spectroscopic orbits for three double-lined binaries, HD 82191 (Am), ω Dra (F5 V), and 108 Her using radial velocities from the 2.1 m telescope at McDonald Observatory, coudé feed Kitt Peak National 2 Fairborn Observatory. The orbital periods range 5.28 to 9.01 days, all systems circular orbits. new dimensions (a1 sin i a2 i) minimum masses (m1 sin3 m2 accuracies of 0.2% or better. Our results confirm large also agree with values previously found Dra. However,...

Abstract T CrB is among the brightest novae. It recurrent with outbursts happening approximately every 80 yr. The next outburst imminent, expected in 2025. binary consists of an M4 III red giant (RG) secondary and a white dwarf (WD) primary. A time series spectra RG was obtained between 2022 2024. Radial velocities (RVs) from these data were combined literature RVs updated orbit computed. circular to high precision has period 227.5494 ± 0.0049 days for solution. An eccentric solution yields...

Numerous infrared spectroscopic observations were obtained of nine asymptotic giant branch (AGB) field M giants that have multiple periods light variability. Each star has a short period several months, which is typical low amplitude pulsation for stars on the AGB, as well long 1–3 yr, significantly longer than predicted fundamental-mode pulsations these stars. The location in AGB period-luminosity relation discussed. For six we found radial-velocity confirm long-period Although considered...

Two unusual Li-rich K giants, HDE 233517 and HD 9746, have been studied. Optical spectroscopy photometry obtained to determine the fundamental parameters of 233517, a single K2 III with an extremely large infrared excess. The spectra yield Teff = 4475 K, log g 2.25, [Fe/H] -0.37, v sin i 17.6 km s-1, non-LTE (7Li) 4.22. Photometric observations reveal low-amplitude light variability period 47.9 days. Combined other parameters, this results in minimum radius 16.7 R☉ distance 617 pc....

We have computed, using 17 infrared radial velocities, the first set of orbital elements for M giant in symbiotic binary V2116 Ophiuchi. The giant's companion is a neutron star, bright X-ray source GX 1+4. rule out previously proposed period 304 days and instead find an 1161 days, by far longest any known binary. orbit has modest eccentricity 0.10, with circularization time ≲5 × 106 yr. large mass function significantly restricts giant. Adopting star 1.35 M☉, maximum 1.22 making it less...

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

HY Vir is found to be a double-lined F0m+F5 binary star with relatively shallow (0.3 mag) partial eclipses. Previous studies of the system are improved 7509 differential photometric observations from URSA WebScope and 8862 NFO WebScope, 68 high-resolution spectroscopic Tennessee State University 2 m automatic telescope, 1 coudé-feed spectrometer at Kitt Peak National Observatory. Very accurate (better than 0.5%) masses radii determined analysis new light curves radial velocity curves....

Time-series spectra of the near-infrared 1.6 μm region have been obtained for five six known D-type symbiotic novae. The map pulsation kinematics Mira component in Mira–white dwarf binary system and provide center-of-mass velocity Mira. No orbital motion is detected agreement with previous estimates periods ≳100 yr semimajor axes ∼50 AU. 1–5 Miras show line weakening during dust obscuration events. This results from scattering continuum emission by 1000 K dust. In heavily obscured HM Sge 4.6...

Abstract The X-ray binary 4U 1954+31 has been classified as a low-mass containing an M giant and neutron star (NS). It also included in the rare class of symbiotic binaries. Gaia parallax, infrared colors, spectral type, abundances, orbital properties demonstrate that cool this system is not but high-mass supergiant. Thus, (HMXB) late-type only known type. mass I <?CDATA ${9}_{-2}^{+6}$?> ⊙ giving age range 12–50 Myr with NS no more than 43 old. spin period one longest known, 5 hr. existence...