108 research outputs found
On the multiplicity of the zero-age main-sequence O star Herschel 36
We present the analysis of high-resolution optical spectroscopic observations
of the zero-age main-sequence O star Herschel 36 spanning six years. This star
is definitely a multiple system, with at least three components detected in its
spectrum. Based on our radial-velocity (RV) study, we propose a picture of a
close massive binary and a more distant companion, most probably in wide orbit
about each other. The orbital solution for the binary, whose components we
identify as O9 V and B0.5 V, is characterized by a period of 1.5415 +/- 0.0006
days. With a spectral type O7.5 V, the third body is the most luminous
component of the system and also presents RV variations with a period close to
498 days. Some possible hypotheses to explain the variability are briefly
addressed and further observations are suggested.Comment: 6 pages, 2 figure
Spectral classification and properties of the O Vz stars in the Galactic O-Star Spectroscopic Survey (GOSSS)
On the basis of the Galactic O-Star Spectroscopic Survey (GOSSS), a detailed
systematic investigation of the O Vz stars is presented. The currently used
spectral classification criteria are rediscussed, and the Vz phenomenon is
recalibrated through the addition of a quantitative criterion based on the
equivalent widths of the He I 4471, He II 4542, and He II 4686 spectral lines.
The GOSSS O Vz and O V populations resulting from the newly adopted spectral
classification criteria are comparatively analyzed. The locations of the O Vz
stars are probed, showing a concentration of the most extreme cases toward the
youngest star forming regions. The occurrence of the Vz spectral peculiarity in
a solar-metallicity environment, as predicted by the fastwind code, is also
investigated, confirming the importance of taking into account several
processes for the correct interpretation of the phenomenon.Comment: Accepted for publication in The Astronomical Journa
The Galactic O-Star Spectroscopic Survey (GOSSS) : III. 142 additional O-type systems
This is the third installment of the Galactic O-Star Spectroscopic Survey (GOSSS), a massive spectroscopic survey of Galactic O stars, based on new homogeneous, high signal-to-noise ratio, R ∼ 2500 digital observations selected from the Galactic O-Star Catalog. In this paper, we present 142 additional stellar systems with O stars from both hemispheres, bringing the total of O-type systems published within the project to 590. Among the new objects, there are 20 new O stars. We also identify 11 new double-lined spectroscopic binaries, 6 of which are of O+O type and 5 of O+B type, and an additional new tripled-lined spectroscopic binary of O+O+B type. We also revise some of the previous GOSSS classifications, present some egregious examples of stars erroneously classified as O-type in the past, introduce the use of luminosity class IV at spectral types O4-O5.5, and adapt the classification scheme to the work of Arias et al.Instituto de Astrofísica de La PlataFacultad de Ciencias Astronómicas y Geofísica
Further Results from the Galactic O-Star Spectroscopic Survey: Rapidly Rotating Late ON Giants
With new data from the Galactic O-Star Spectroscopic Survey, we confirm and
expand the ONn category of late-O, nitrogen-enriched (N), rapidly rotating (n)
giants. In particular, we have discovered two "clones" (HD 102415 and HD
117490) of one of the most rapidly rotating O stars previously known (HD
191423, "Howarth's Star"). We compare the locations of these objects in the
theoretical HR Diagram to those of slowly rotating ON dwarfs and supergiants.
All ON giants known to date are rapid rotators, whereas no ON dwarf or
supergiant is; but all ON stars are small fractions of their respective
spectral-type/luminosity-class/rotational subcategories. The ONn giants,
displaying both substantial processed material and high rotation at an
intermediate evolutionary stage, may provide significant information about the
development of those properties. They may have preserved high initial
rotational velocities or been spun up by TAMS core contraction; but
alternatively and perhaps more likely, they may be products of binary mass
transfer. At least some of them are also runaway stars.Comment: 18 pages, 2 figures, 2 tables; accepted for publication in the
November 2011 issue of The Astronomical Journa
Spectral classification and properties of the O VZ stars in the Galactic O-Star Spectroscopic Survey (GOSSS)
On the basis of the Galactic O Star Spectroscopic Survey (GOSSS), we present a detailed systematic investigation of the O Vz stars. The currently used spectral classification criteria are rediscussed, and the Vz phenomenon is recalibrated through the addition of a quantitative criterion based on the equivalent widths of the He i λ4471, He ii λ4542, and He ii λ4686 spectral lines. The GOSSS O Vz and O V populations resulting from the newly adopted spectral classification criteria are comparatively analyzed. The locations of the O Vz stars are probed, showing a concentration of the most extreme cases toward the youngest star-forming regions. The occurrence of the Vz spectral peculiarity in a solar-metallicity environment, as predicted by the fastwind code, is also investigated, confirming the importance of taking into account several processes for the correct interpretation of the phenomenon.Instituto de Astrofísica de La PlataFacultad de Ciencias Astronómicas y Geofísica
He II λ4686 in η Carinae: Collapse of the wind-wind collision region during periastron passage
The periodic spectroscopic events in η Carinae are now well established and occur near the periastron passage of two massive stars in a very eccentric orbit. Several mechanisms have been proposed to explain the variations of different spectral features, such as an eclipse by the wind-wind collision (WWC) boundary, a shell ejection from the primary star or accretion of its wind onto the secondary. All of them have problems explaining all the observed phenomena. To better understand the nature of the cyclic events, we performed a dense monitoring of η Carinae with five Southern telescopes during the 2009 low-excitation event, resulting in a set of data of unprecedented quality and sampling. The intrinsic luminosity of the He II λ4686 emission line (L 310 L) just before periastron reveals the presence of a very luminous transient source of extreme UV radiation emitted in the WWC region. Clumps in the primary's wind probably explain the flare-like behavior of both the X-ray and He II λ4686 light curves. After a short-lived minimum, He II λ4686 emission rises again to a new maximum, when X-rays are still absent or very weak. We interpret this as a collapse of the WWC onto the "surface" of the secondary star, switching off the hard X-ray source and diminishing the WWC shock cone. The recovery from this state is controlled by the momentum balance between the secondary's wind and the clumps in the primary's wind.Facultad de Ciencias Astronómicas y Geofísica
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