Оглавление
Изображения
Загрузить ваше изображение
DSS Images Other Images
Публикации по объекту
Spectral Classification of Stars in A Supplement to the Bright Star Catalogue
MK spectral types are given for about 584 stars in A Supplement to theBright Star Catalogue. These are compared with Hipparcos parallaxes tocheck the reliability of those classifications. The estimated errors are+/-1.2 subtypes, and 10% of the luminosity classes may be wrong.
| Close frequency pairs in Delta Scuti stars
The majority of the well-studied delta Scuti stars shows frequency pairsin the power spectra with frequency separations less than 0.06cd-1 (0.7 mu Hz) as well as amplitude variability. We examinethe interpretation in terms of separate excited stellar pulsation modes,single modes with variable amplitudes, and observational problems. Thevariable-phase technique, which examines the phase jumps near the timesof minimum amplitude of an assumed single frequency, is applied to theextensive data of the star BI CMi, which shows some of the most extremebehavior. The following results are found for the 5 features in thepower spectrum which could be explained as single modes with variableamplitudes or as double modes: for three features it can be shown thatthese are indeed pairs of separate pulsation modes beating with eachother: at times of minimum amplitude the phase jumps are observed andboth the observed amplitude and phase variations can be predictedcorrectly by assuming two separate modes of nearly equal frequencies.Artifacts caused by observational error, insufficient frequencyresolution or variable amplitudes can be ruled out. A fourth pair has aprobable origin in two excited modes, while a 5th case is inconclusivedue to long time scales of variability and small amplitudes. Theexistence of close frequency needs to be taken into account in planningthe lengths of earth-based as well as space campaigns so that sufficientfrequency resolution is obtained. Possible reasons for the existence ofclose frequencies in delta Scuti stars are considered. They include thedense frequency spacing caused by the presence of mixed modes,rotational splitting as well as near-coincidence of the frequencies ofmodes with different l values (the so-called Small Spacing).
| A revised catalogue of delta Sct stars
An extensive and up-dated list of delta Sct stars is presented here.More than 500 papers, published during the last few years, have beenrevised and 341 new variables have been added to our last list, sixyears ago. This catalogue is intended to be a comprehensive review onthe observational characteristics of all the delta Sct stars known untilnow, including stars contained in earlier catalogues together with othernew discovered variables, covering information published until January2000. In summary, 636 variables, 1149 references and 182 individualnotes are presented in this new list. Tables 1 and 2 will be accessibleonly in electronic form at the CDS via anonymous ftp tocdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html
| CCD photometry of a delta Scuti variable in an open cluster. III. V 465 Persei in the alpha Persei cluster
We present the results of real-time CCD differential photometry for thedelta Scuti variable V 465 Per. The observations were performed forthirteen nights between November, 1994 and January, 1995. Total 3345points of differential V magnitudes were collected during theobservation period of 76.4 hours. From the Fourier analysis, we havedetected four frequencies as follows; f_1=14.040 c/d, f_2=17.208 c/d,f_3=33.259 c/d and f_4=13.721 c/d. Two frequencies of 12.50 c/d and33.49 c/d detected previously by Slovak (1978, ApJ 223, 192) maycorrespond to our f_1 and f_3, respectively. For each frequency,pulsation constants of Q_1=0.0520+/-0.008, Q_2=0.0425+/-0.006,Q_3=0.0220+/-0.003 and Q_4=0.0533+/-0.008 were derived from severalobservational properties of V 465 Per. Only the value of Q_3 is found tobe within the range of theoretical p-mode oscillations and the otherones show large differences relative to the theoretical values. The highQ-values might be interpreted as the occurrence of g-mode oscillationsin V 465 Per, even though it can not rule out the possibility ofsystematic errors (Breger 1990; Delta Scuti Star Newsletter, 2, 13)related to rotational velocity.
| Frequency analysis of the light curve of the δ Scuti star HD 74292
Not Available
| A catalogue of variable stars in the lower instability strip.
Identifications, positions, photometry, spectra, some pulsationalfeatures, other astrophysical parameters and literature for 302pulsating variable stars in the lower instability strip, near the ZAMS,are given. About 185 stars have near homogeneous photometric informationin the Stroemgren's uvby-β photometric system. Thiscatalogue/database covers information published until November 1993.
| Main Sequence Variables
The pulsators along and near the main sequence are well-suited forasteroseismology and provide a probe of the stellar interior and itschanges with evolution. With the exception of rapidly oscillating Apstars (roAp), the pulsation periods range from 0.5 h to days. Thisrequires multisite campaigns lasting several weeks. The delta Scuti,roAp and beta Cephei variables offer the greatest potential, while thelonger-period g-mode pulsators (SPB -- slowly pulsating B stars -- andgamma Doradus variables) are very difficult to study. A summary of themultiperiod structure of delta Scuti stars is given. The twobest-studied stars, FG Vir and CD--24(deg) 7599, both have been WETtargets. A preliminary analysis of the 1995 campaign of FG Vir hasalready detected 19 frequencies. The standard photometric WET techniquehas a high duty cycle since the variable star is observed continuouslywith one channel. The study of main sequence variables requiresphotometric stability at low frequencies. The extension of the WETtechnique to low frequencies and its modification are discussed.
| First radial velocities for 146 bright F- and G-type stars
We have obtained an average of 5.7 radial velocities for 146 northernstars of types F and G (all luminosity classes) listed in 'A Supplementto the Bright Star Catalogue' as having no previously known radialvelocity measures. Those were obtained with charge coupled devices(CCDs) and a cross-correlation technique; the intrinsic velocityaccuracy, based on stars of apparently constant velocity, is probablyless than +/- 0.3 km/s per mean. Of those stars 14% are newly discoveredSB2 stars. The prevelance of rapid profile variations (in minutes orhours) in most of the broad-lined F-type stars makes it difficult toobtain accurate measures for them.
| Multi-period pulsation of the delta Scuti star 63 Herculis
Multisite photoelectric B and V photometry of the delta Scuti star 63Her was obtained on three continents. Three frequencies of pulsation(f1 = 11.32, f2 = 20.07 and f3 = 7.72c/d) were detected with a signal/noise amplitude ratio greater than or =4.0. The three frequencies fit all the available data ranging back to1968. Reports in the literature of discepant behavior of the 1968measurements were probably caused by overinterpretation. The newfrequency values are in excellant agreement with the results found byReed & Welch from their 1983 data, except for a 1 c/d alias in theirvalue for f2. Two additional pulsation frequencies in thelow-frequency g-mode domain with amplitudes near two millimag reportedby the STEPHI group are not seen in the new campaign data. The new datashow average noise levels just below one millimag in this frequencydomain, so that the existence of these two frequencies cannot bedisproved from the new data alone. However, a reanalysis of the STEPHIdata also suggests that these frequencies might not be real. The resultsfrom the two multisite campaigns should be free of 1 c/d aliasing, sothat a resonance hypothesis involving f2 = f1 +f3 can be rejected. The value of the pulsation constantassociated with f3, Q = 0.046 +/- 0.008 d, is too high by 2standard deviations to be explained by radial pulsation. The Q value isincompatible with those of nonradial p1 to p4modes commonly found in delta Scuti stars.
| δ Scuti stars: a new revised list
An extensive and up to date list of δ Sct stars is presented. Thiscatalogue is intended to be a comprehensive review of observationalcharacteristics of all the δ Sct stars known until now, includingstars contained in earlier catalogues together with other new discoveredvariables, covering information published until November 1993. Globalinformation in the form of histograms and diagrams are also shown.
| Insight into the Pulsational Behaviour of δ Scuti Stars
Not Available
| Pulsational Behaviours of the Delta-Scuti Stars HD18878 and HD19279
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1993A&A...274..811M&db_key=AST
| The 71st Name-List of Variable Stars
Not Available
| The radial velocity curve and the two-dimensional spectral classification of the Delta SCT variable HD 18878
The radial velocities of HD 18878 were measured from spectra of this newDelta Sct type variable. The radial velocity curve with elementsdetermined from the photoelectric observations of Frolov et al. (1990)is derived. The mean radial velocity is -20 km/s, and the amplitude ofits variation is 34 km/s. On the basis of spectral criteria and thelocation of this star on a two-color diagram, it is argued that HD 18878is an A9III star.
| Doing research with small telescopes : frequency analysis of multiperiodic delta Scuti stars.
Not Available
| A New, Apparently Unusual delta Scuti Star, HD 18878
Not Available
| Stars Brighter than V=6M5 not Listed in the HR Catalogue
Not Available
|
Добавить новую статью
Внешние ссылки
- - Внешних ссылок не найдено -
Добавить внешнюю ссылку
Группы:
|
Наблюдательные данные и астрометрия
| Созвездие: | Персей |
| Прямое восхождение: | 03h03m56.74s |
| Склонение: | +47°50'54.5" |
| Видимая звёздная величина: | 6.474 |
| Расстояние: | 111.483 парсек |
| Собственное движение RA: | -8.6 |
| Собственное движение Dec: | -6.9 |
| B-T magnitude: | 6.79 |
| V-T magnitude: | 6.501 |
Каталоги и обозначения:
|
INHABITED SKY
