High Velocity Spectroscopic Binary Orbits from Photoelectric Radial Velocities: BD+20 5152, a Possible Triple System

2010 ◽  
Vol 19 (3-4) ◽  
Author(s):  
J. Sperauskas ◽  
A. Bartkevičius ◽  
R. P. Boyle ◽  
V. Deveikis
Keyword(s):  
Radial Velocity ◽  
Proper Motion ◽  
High Velocity ◽  
Triple System ◽  
Mass Velocity ◽  
Center Of Mass ◽  
Primary Component ◽  
Eccentric Orbit ◽  
Velocity Measurements ◽  
Spectroscopic Binary

AbstractThe spectroscopic orbit of a high proper motion star, BD+20 5152, is calculated from 34 CORAVEL-type radial velocity measurements. The star has a slightly eccentric orbit with a period of 5.70613 d, half-amplitude of 47.7 km/s and eccentricity of 0.049. The center-of-mass velocity of the system is -24.3 km/s. BD+20 5152 seems to be a triple system consisting of a G8 dwarf as a primary component and of two K6-M0 dwarfs as secondary and tertiary components. This model is based on the analysis of its UBVRI and JHK magnitudes. According to the SuperWASP photometry, spots on the surface of the primary are suspected. The excessive brightness in the Galex FUV and NUV magnitudes and a non-zero eccentricity suggest the age of this system to be less than 1 Gyr.

scholarly journals The Structure of the HH39 Region

1987 ◽  
Vol 115 ◽  
pp. 340-341
Author(s):  
J. R. Walsh
Keyword(s):  
High Resolution ◽  
Radial Velocity ◽  
Proper Motion ◽  
High Velocity ◽  
Velocity Structure ◽  
The Other ◽  
Emission Lines ◽  
High Resolution Spectroscopy ◽  
Bow Shocks ◽  
Hh Objects

HH39 is the group of Herbig-Haro (HH) objects associated with the young semi-stellar object R Monocerotis (R Mon) and the variable reflection nebula NGC 2261. An R CCD frame and a B prime focus plate of the region show a filament connecting NGC 2261 with HH39, confirming the association between R Mon and the HH objects. This filament is probably composed of emission material. The southern knot in HH39 has brightened over the last 20 years; its proper motion has been determined and is similar to that of the other knots. A total of 8 knots can be distinguished in HH39 surrounded by diffuse nebulosity. High resolution spectroscopy of the Hα and [N II] emission lines shows the spatial variation of the radial velocity structure over the largest knots (HH39 A and C). Distinct differences in excitation and velocity structure between the knots are apparent. The observations are compatible with the knots being high velocity ejecta from R Mon, decelerated by interaction with ambient material and with bow shocks on their front surfaces.

scholarly journals Proxima’s orbit around α Centauri

2017 ◽  
Vol 598 ◽  
pp. L7 ◽  
Author(s):  
P. Kervella ◽  
F. Thévenin ◽  
C. Lovis
Keyword(s):  
Radial Velocity ◽  
High Precision ◽  
Orbital Period ◽  
Triple System ◽  
Orbital Motion ◽  
The Sun ◽  
Proper Motions ◽  
Velocity Measurements ◽  
Degree Of Confidence ◽  
High Degree

Proxima and α Centauri AB have almost identical distances and proper motions with respect to the Sun. Although the probability of such similar parameters is, in principle, very low, the question as to whether they actually form a single gravitationally bound triple system has been open since the discovery of Proxima one century ago. Owing to HARPS high-precision absolute radial velocity measurements and the recent revision of the parameters of the α Cen pair, we show that Proxima and α Cen are gravitationally bound with a high degree of confidence. The orbital period of Proxima is ≈ 550 000 yr. With an eccentricity of 0.50+0.08-0.09, Proxima comes within 4.3+1.1-0.9 kau of α Cen at periastron, and is currently close to apastron (13.0+0.3-0.1 kau). This orbital motion may have influenced the formation or evolution of the recently discovered planet orbiting Proxima, as well as circumbinary planet formation around α Cen.

scholarly journals Membership status of TWA22AB

2009 ◽  
Vol 5 (S266) ◽  
pp. 540-543
Author(s):  
Ramachrisna Teixeira ◽  
Christine Ducourant ◽  
Gael Chauvin ◽  
Alberto G. O. Krone–Martins ◽  
Mickael Bonnefoy ◽  
...  
Keyword(s):  
Radial Velocity ◽  
Proper Motion ◽  
Velocity Measurements ◽  
Trigonometric Parallax

AbstractUsing the ESO NTT/SUSI2 telescope, we observed TWA22AB during five different observing runs over 1.2 years to measure its trigonometric parallax and proper motion. HARPS at the ESO 3.6m telescope was also used to measure the system's radial velocity over 2 years. Based on trigonometric-parallax, proper-motion and radial-velocity measurements, we re-analyzed the membership of TWA22AB of the young, nearby associations TW Hydrae, β Pictoris and Tucana–Horologium.

scholarly journals WIYN Open Cluster Study. LXXXII. Radial-velocity Measurements and Spectroscopic Binary Orbits in the Open Cluster NGC 7789

2020 ◽  
Vol 160 (4) ◽  
pp. 169 ◽  
Author(s):  
Andrew C. Nine ◽  
Katelyn E. Milliman ◽  
Robert D. Mathieu ◽  
Aaron M. Geller ◽  
Emily M. Leiner ◽  
...  
Keyword(s):  
Radial Velocity ◽  
Open Cluster ◽  
Velocity Measurements ◽  
Spectroscopic Binary

scholarly journals Radial velocity measurements and orbit determination of eight single-lined spectroscopic binary systems

2017 ◽  
Vol 338 (6) ◽  
pp. 671-679 ◽  
Author(s):  
R. Bischoff ◽  
M. Mugrauer ◽  
T. Zehe ◽  
D. Wöckel ◽  
A. Pannicke ◽  
...  
Keyword(s):  
Radial Velocity ◽  
Orbit Determination ◽  
Binary Systems ◽  
Velocity Measurements ◽  
Spectroscopic Binary

scholarly journals Radial Velocities of SS Cygni

1979 ◽  
Vol 53 ◽  
pp. 489-493
Author(s):  
R. J. Stover
Keyword(s):  
Radial Velocity ◽  
Emission Line ◽  
Absorption Line ◽  
Orbital Period ◽  
Radial Velocities ◽  
Orbital Elements ◽  
Velocity Measurements ◽  
Light Spectrum ◽  
Minimum Light ◽  
Spectroscopic Binary

SS Cygni was found by Joy (1956) to be a spectroscopic binary with an orbital period of about 6-1/2 hours. At minimum light it has mv=12 and is the brightest member of the dwarf nova class of variables. The minimum light spectrum reveals faint, narrow absorption lines of a G- or K-type star along with strong, broad emission lines of hydrogen, helium, and calcium which are produced by an accretion disk surrounding a white dwarf star. Joy’s radial velocities were not very accurate. Nevertheless, he was able to estimate the orbital elements, finding 115 km/s for the absorption line K-velocity and 122 km/s for the emission line K-velocity. In addition, he derived an orbital period of 0276244. Later minimum light observations by Walker and Chincarini (1968) were too few to be able to improve the orbital elements. Kiplinger (1979) refined the emission line radial velocities but was not able to remeasure the faint absorption line spectrum. This paper presents new radial velocity measurements of both the emission and absorption line spectra of SS Cygni at minimum light, and is the first thorough investigation of this star’s radial velocity variations in more than 20 years. The accuracy of the radial velocity curves has been greatly improved. We also find that Joy’s orbital period is in error by nearly two minutes.

scholarly journals A New, Young, Low-Mass Spectroscopic Binary Without a Home

2015 ◽  
Vol 10 (S314) ◽  
pp. 65-66
Author(s):  
Laura S. Flagg ◽  
Evgenya L. Shkolnik ◽  
Alycia J. Weinberger ◽  
Brendan P. Bowler ◽  
Adam L. Kraus ◽  
...  
Keyword(s):  
Radial Velocity ◽  
Dimensional Space ◽  
Three Dimensional ◽  
Young Star ◽  
Proper Motions ◽  
Velocity Measurements ◽  
Spectroscopic Binary ◽  
Low Mass ◽  
Three Dimensional Space

AbstractWe have discovered that 2MASS 08355977-3042306 is an accreting K7, double-lined, spectroscopic binary younger than ~20 Myr. The age of a dispersed young star can best be determined if it is a member of a known young moving group. However, the three dimensional space velocities (UVW) we calculate using radial velocity measurements, proper motions, and plausible photometric distances make membership in any known young moving group unlikely.

scholarly journals The Arches cluster revisited

2018 ◽  
Vol 617 ◽  
pp. A66 ◽  
Author(s):  
M. E. Lohr ◽  
J. S. Clark ◽  
F. Najarro ◽  
L. R. Patrick ◽  
P. A. Crowther ◽  
...  
Keyword(s):  
Radial Velocity ◽  
Survey Data ◽  
Massive Stars ◽  
Primary Component ◽  
Initial Mass ◽  
Binary Interaction ◽  
Evolutionary Stage ◽  
Eccentric Orbit ◽  
X Ray ◽  
The Galaxy

We have carried out a spectroscopic variability survey of some of the most massive stars in the Arches cluster, using K-band observations obtained with SINFONI on the VLT. One target, F2, exhibits substantial changes in radial velocity (RV); in combination with new KMOS and archival SINFONI spectra, its primary component is found to undergo RV variation with a period of 10.483 ± 0.002 d and an amplitude of ~350 km s−1. A secondary RV curve is also marginally detectable. We reanalysed archival NAOS-CONICA photometric survey data in combination with our RV results to confirm this object as an eclipsing SB2 system, and the first binary identified in the Arches. We have modelled it as consisting of an 82 ± 12 M⊙ WN8–9h primary and a 60 ± 8 M⊙ O5–6 Ia+ secondary, and as having a slightly eccentric orbit, implying an evolutionary stage prior to strong binary interaction. As one of four X-ray bright Arches sources previously proposed as colliding-wind massive binaries, it may be only the first of several binaries to be discovered in this cluster, presenting potential challenges to recent models for the Arches’ age and composition. It also appears to be one of the most massive binaries detected to date; the primary’s calculated initial mass of ≳120 M⊙ would arguably make this the most massive binary known in the Galaxy.

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