Statistical analysis of intrinsic polarization, IR excess and projected rotational velocity distributions of classical Be stars
We present the results of statistical analyses of a sample of 627 Bestars. The parameters of intrinsic polarization (p*),projected rotational velocity (v sin i), and near IR excesses have beeninvestigated. The values of p* have been estimated for a muchlarger and more representative sample of Be stars (~490 objects) thanpreviously. We have confirmed that most Be stars of early spectral typehave statistically larger values of polarization and IR excesses incomparison with the late spectral type stars. It is found that thedistributions of p* diverge considerably for the differentspectral subgroups. In contrast to late spectral types (B5-B9.5), thedistribution of p* for B0-B2 stars does not peak at the valuep*=0%. Statistically significant differences in the meanprojected rotational velocities (/line{vsin i}) are found for differentspectral subgroups of Be stars in the sense that late spectral typestars (V luminosity class) generally rotate faster than early types, inagreement with previously published results. This behaviour is, however,not obvious for the III-IV luminosity class stars. Nevertheless, thecalculated values of the ratio vt/vc of the truerotational velocity, vt, to the critical velocity forbreak-up, vc, is larger for late spectral type stars of allluminosity classes. Thus, late spectral type stars appear to rotatecloser to their break-up rotational velocity. The distribution of nearIR excesses for early spectral subgroups is bi-modal, the position ofthe second peak displaying a maximum value E(V-L)~ 1 . m 3for O-B1.5 stars, decreasing to E(V-L)~0. m8 for intermediatespectral types (B3-B5). It is shown that bi-modality disappears for latespectral types (B6-B9.5). No correlations were found betweenp* and near IR excesses and between E(V-L) and vsin i for thedifferent subgroups of Be stars. In contrast to near IR excesses, arelation between p* and far IR excesses at 12 mu m is clearlyseen. A clear relation between p* and vsin i (as well asbetween p* and /line{vsin i}/vc) is found by thefact that plots of these parameters are bounded by a ``triangular"distribution of p*: vsin i, with a decrease of p*towards very small and very large vsin i (and /line{vsini}/vc) values. The latter behaviour can be understood in thecontext of a larger oblateness of circumstellar disks for the stars witha rapid rotation. From the analysis of correlations between differentobservational parameters we conclude that circumstellar envelopes forthe majority of Be stars are optically thin disks with the range of thehalf-opening angle of 10degr
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Rotational Velocity Determinations for 164 Be and B Stars
Rotational velocities, v sin i, have been obtained for 96 Be and 68normal B stars by measurements of the FWHM of the He I lambda-4471 line(for spectral types B0-B4.5) and Mg II lambda-4481 (for types B5-B9.5).The consistency of various published sources is examined. (SECTION:Stars)
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Be-Stars and Shell Stars Observed with the 13-COLOR Photometric System - Part Two
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1984RMxAA...9..141S&db_key=AST
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A second catalog of the profile of the H-alpha line in 55 Be stars
A second catalog of the H-alpha line profile of 55 Be stars ispresented, thereby raising the total H-alpha line profiles for Be starsto 127 stars. The measurements were made with the echelle spectrographon the 152 cm telescope at the Haute Provence Observatory. Photosphericabsorption was dominant in 12 percent of the stars, and not visible atall in 64 percent of the objects, where H-alpha and H-beta radiationwere combined. A central absorption for the H-alpha emission wasdetected in 73 percent of the cases, and FWHM emission intensities werecorrelated with the rotational velocities of the stars. The group I Bestars displayed emission lines which were not detectable of stars ofother groupings.
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Thirteen-color photometry of Be stars
Thirteen-color photometry made at the San Pedro Matir Observatory inBaja California for a number of spectroscopically variable Be and shellstars is presented. Several of these stars show photometric variabilityin the UV and/or IR over a time base of two to three years. The moreinteresting stars are analyzed in terms of color-color diagrams, colorexcesses, spectral characteristics and changes in their energydistributions. Prospects for future research are discussed.
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A classification of Be stars
Based upon a sample of 140 stars observed over 20 years for which about5,000 spectrograms are available, a classification scheme of Be stars ispresented. This is the first attempt to subdivide the Be star group intophysically significant subgroups, from which typical objects can beselected for further study. The four groups proposed are based upon adiscussion of spectrum characteristics, multicolor photometry,polarization, rotational velocities, UV spectral types and timevariability. Starting with the group membership of a Be star,predictions can be made of the future behavior of it.
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Absolute ultraviolet spectrophotometry with the TD-1 satellite. XI - Spectrophotometric study of Be and shell stars with the S 2/68 experiment
Low resolution S 2/68 observations are used to show that Be stars ofspectral type B0-B5 have a deficiency of ultraviolet radiation (at 2100A) as compared to the visible with respect to normal stars of the samespectral type. The deficiency is statistically correlated with thestrength of visual emission lines, with the existence of an infraredexcess and with the presence of a shell. Comparison criteria for Be andB stars are discussed along with the relation between the interstellarcolor excess and the depth of the 2200 A absorption feature for normal Bstars. In addition, the origin of the flux deficiency is considered, andit is shown that the stars with a shell of hydrogen and metals (a strongshell) have a source of absorption different from that of the Be starswith strong emission.
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Photoelectric measures of the hydrogen lines in early-type stars.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1974MNRAS.169..171F&db_key=AST
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Etudes d'etoiles Be-decrements Balmer.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1971A&A....11...57B&db_key=AST
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A Spectroscopic and Photometric Study of the be Stars.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1958ApJ...128..207M&db_key=AST
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Supplement to the Mount Wilson Catalogue and Bibliography of Stars of Classes B and a whose Spectra have Bright Hydrogen Lines.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1943ApJ....98..153M&db_key=AST
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Discovery and Observations of Stars of Class Be. Third Paper.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1942ApJ....96...15M&db_key=AST
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INHABITED SKY
