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Publisher: Springer-Verlag   (Total: 2341 journals)

 Astrophysical Bulletin   [SJR: 0.469]   [H-I: 11]   [2 followers]  Follow         Hybrid journal (It can contain Open Access articles)    ISSN (Print) 1990-3421 - ISSN (Online) 1990-3413    Published by Springer-Verlag  [2341 journals]
• Ultra-flat galaxies selected from RFGC catalog. III. Star formation rate
• Authors: O. V. Melnyk; V. E. Karachentseva; I. D. Karachentsev
Pages: 1 - 15
Abstract: Abstract We examine the star formation properties of galaxies with very thin disks selected from the Revised FlatGalaxy Catalog (RFGC). The sample contains 333 ultra-flat galaxies (UFG) at high Galactic latitudes, b > 10◦, with a blue major angular diameter of a ≥ 1.'2, blue and red apparent axial ratios of (a/b)b > 10, (a/b)r > 8.5 and radial velocities within 10 000 kms−1. As a control sample for them we use a population of 722 more thick RFGC galaxies with (a/b)b > 7, situated in the same volume. The UFG distribution over the sky indicates them as a population of quite isolated galaxies.We found that the specific star formation rate, sSFR FUV, determined via the FUV GALEX flux, increases steadily from the early type to late type disks for both the UFG and RFGC–UFG samples, showing no significant mutual difference within each morphological type T. The population of UFG disks has the average HI-mass-to-stellarmass ratio by (0.25 ± 0.03) dex higher than that of RFGC–UFG galaxies. Being compared with arbitrary orientated disks of the same type, the ultra-flat edge-on galaxies reveal that their total HI mass is hidden by self-absorption on the average by approximately 0.20 dex.We demonstrate that using the robust stellar mass estimate via 〈B−K〉-color and galaxy type T for the thin disks, together with a nowaday accounting for internal extinction, yields their sSFR quantities definitely lying below the limit of −9.4 dex (yr−1). The collected observational data on UFG disks imply that their average star formation rate in the past has been approximately three times the current SFR. The UFG galaxies have also sufficient amount of gas to support their observed SFR over the following nearly 9 Gyrs.
PubDate: 2017-01-01
DOI: 10.1134/s1990341317030014
Issue No: Vol. 72, No. 1 (2017)

• Stars with discrepant v sin i as derived from the Ca II 3933 and Mg II
4481 Å lines. VI. HD 199892 — an SB2 spectroscopic binary
• Authors: J. Zverko; I. Romanyuk; I. Iliev; D. Kudryavtsev; I. Stateva; E. Semenko
Pages: 16 - 23
Abstract: Abstract We analyzed the spectra of a well known SB1 binary HD199892 for which the projected rotational velocity v sin i, introduced in the literature, significantly differs when determined from the lines of Ca II at 3933 Å and ofMg II at 4481 Å. Contrary to the former findings, we discovered the signs of spectral lines of a companion star in the profile of Hβ as well as weak metallic lines in the high resolution high S/N spectra covering the most of the visual region. We estimated the secondary star to be a main sequence A4V star with a mass of 2.2M ⊙ and derived its radial velocity which resulted in the mass of the primary M = 4.6M ⊙. Short sections of the spectra in the Mg II 4481 Å and Ca II 3933 Å regions are analyzed as well.
PubDate: 2017-01-01
DOI: 10.1134/s1990341317030026
Issue No: Vol. 72, No. 1 (2017)

• Physical and geometrical parameters of CVBS. XII. FIN 350 (HIP 64838)
• Authors: M. A. Al-Wardat; J. A. Docobo; A. A. Abushattal; P. P. Campo
Pages: 24 - 34
Abstract: Abstract A complete astrophysical and dynamical study of the close visual binary system (CVBS) Finsen 350 (A7V + F0V), is presented. Beginning with the entire observational spectral energy distribution (SED) and the magnitude difference between the subcomponents, Al-Wardat’s complex method for analyzing CVBS was applied as a reverse method of building the individual and entire synthetic SEDs of the system. This was combined with Docobo’s analytic method to calculate the new orbits. Although possible short (approximately 9 years) and long period (of about 18 years) orbits could be considered taking into account the similar results of the stellar masses obtained for each of them (3.07 and 3.41 M ⊙, respectively), we confirmed that the short solution is correct. In addition, other physical, geometrical and dynamical parameters of this system such as the effective temperatures, surface gravity accelerations, absolute magnitudes, radii, the dynamical parallax, etc., are reported. The Main Sequence phase of both components with age around 0.79 Gyr is approved.
PubDate: 2017-01-01
DOI: 10.1134/s1990341317030038
Issue No: Vol. 72, No. 1 (2017)

• Study of nonstationarity of the atmosphere of κ Cas. I. Variability of
profiles of photospheric and He I wind lines
• Authors: A. Kh. Rzaev
Pages: 35 - 43
Abstract: Abstract Temporal variations of radial velocities and line profiles in the spectrum of the supergiant κ Cas were investigated. Variability of radial velocities and profiles of photospheric lines Si III, OII, He I, H10–Hδ and wind lines He I λ 5875, 6678 Å ismainly caused by non-radial pulsations. For photospheric lines quasisinusoidal variabilities of the radial velocity were found. Temporal variability of radial velocity of the wind lines He I λ 5875, 6678 A˚ differ from each other and from the photospheric lines. Gamma velocities and amplitudes of radial velocity variability were determined. The amplitude of variability and the velocity of expansion increase from lower to upper layers of the atmosphere. Emission components are superimposed on the line profiles at positions about −135 ± 10.0, −20 ± 20 and 135 ± 10.0 kms−1 respectively. They are more obvious in the wind line profiles, although, there are signs of emissions also in the photospheric lines. Such a character of variability of all the lines in the κ Cas spectrum confirms its Be nature.
PubDate: 2017-01-01
DOI: 10.1134/s199034131703004x
Issue No: Vol. 72, No. 1 (2017)

• Search for and study of photometric variability in magnetic white dwarfs
• Authors: A. F. Valeev; K. A. Antonyuk; N. V. Pit; A. S. Moskvitin; A. O. Grauzhanina; D. R. Gadelshin; S. V. Kolesnikov; E. A. Zhuzhulina; T. E. Burlakova; G. A. Galazutdinov; A. G. Gutaev; R. Ya. Zhuchkov; A. I. Ikhsanova; D. G. Zhukov; Arti Joshi; J. C. Pandey; A. F. Kholtygin; G. G. Valyavin
Pages: 44 - 50
Abstract: Abstract We report the results of photometric observations of a number of magnetic white dwarfs in order to search for photometric variability in these stars. These V-band observations revealed significant variability in the classical highly magnetized white dwarf GRW+70◦8247 with a likely period from several days to several dozen days and a half-amplitude of about 0. m 04. Our observations also revealed the variability of the well-known white dwarf GD229. The half amplitude of its photometric variability is equal to about 0. m 005, and the likely period of this degenerate star lies in the 10–20 day interval. This variability is most likely due to the rotation of the stars considered.We also discuss the peculiarities of the photometric variability in a number of other white dwarfs. We present the updated “magnetic field–rotation period” diagram for the white dwarfs.
PubDate: 2017-01-01
DOI: 10.1134/s1990341317030051
Issue No: Vol. 72, No. 1 (2017)

• Estimates of the radii, masses, and luminosities of LAMOST stars
• Authors: S. G. Sichevskij
Pages: 51 - 57
Abstract: Abstract Based on the spectral observations of the LAMOST (DR2) survey, the radii, masses, and luminosities of 700 481 stars were estimated. These stars belong to spectral types A, F, G, and K, and have metallicities between −0.845 and 0.0. To determine the properties of the stars, we used up-to-date models of the stellar interior structure, computed with account for the stellar evolution rate and the initial mass function. The use of evolutionary estimates for two types of stars—with and without rotation—allowed us to account for the uncertainty associated with the lack of data on the rotation velocity of the stars under consideration. The obtained stellar radii, together with the photometric estimates of interstellar extinction and angular diameters can be used to study the dependence of interstellar extinction on distance as well as to estimate the stellar distances.
PubDate: 2017-01-01
DOI: 10.1134/s1990341317030063
Issue No: Vol. 72, No. 1 (2017)

• Spectrum and physical conditions in microflare generation regions at
decimeter-wave frequencies
• Authors: L. V. Yasnov; V. M. Bogod; A. A. Gofman; O. M. Stupishina
Pages: 58 - 66
Abstract: Abstract The event of March 11, 2011 was used to study decimeter-wave microflares (MF) in solar active regions. A theoretical interpretation has been proposed for the nature and generation mechanism of decimeter-waveMFs, which is based on an analysis of the phenomenon of double plasma resonance and subsequent transformation of upper hybrid waves when they interact with low-frequency plasma waves. It is shown that MFs should form in the active regions between magnetic fields of opposite direction, where magnetic-field strength reaches 100–150 G in the transition region. We report the spectral properties of MFs computed with the allowance for inverse bremsstrahlung and cyclotron absorption and for the increment of upper-hybrid waves. It is shown that the transition region is the most likely place of MF generation within the framework of the model of electron-density and temperature. It is also shown that within the framework of electron density and temperature model in the active region the most likely MF generation place in the solar atmosphere is the transition region. MFs were observed at frequencies from 1.036 to 1.306 Hz, which is consistent with model computations.
PubDate: 2017-01-01
DOI: 10.1134/s1990341317030075
Issue No: Vol. 72, No. 1 (2017)

• Spectroscopic observations of the exoplanet WASP-32b transit
• Authors: A. O. Grauzhanina; G. G. Valyavin; D. R. Gadelshin; D. N. Baklanova; S. I. Plachinda; K. A. Antonyuk; N. V. Pit; G. A. Galazutdinov; A. F. Valeev; T. E. Burlakova; A. F. Kholtygin
Pages: 67 - 72
Abstract: Abstract We present first results of spectroscopic observations of transiting exoplanets in the Special Astrophysical Observatory of the Russian Academy of Sciences with the Main Stellar Spectrograph of the 6-m BTA telescope. For the exoplanetWASP-32b, we detected a significant variation of intensity and equivalent width in the Hα spectral line of the parent star at the time of a transit. The equivalent width of the line during transit is by 8–10% larger than outside the planet passage. Residual intensity in the core of the line reveals the following tendency: the line is by 10–15% deeper inside transit than outside it. Observations with the long-slit spectrograph of the Crimean Astrophysical Observatory at the 2.6-m ZTSh telescope also showed a transit event in the Hα line, although, with a smaller amplitude and shape inverted in relation to the data from the 6-m telescope. While in the observations with the BTA the Hα line becomes deeper during the transit, in the ZTSh observations, the residual intensity of the Hα line decreases during the transit. Reducing and analysis of the archive data of WASP-32b observations with the HARPS spectrograph also confirm the Hα line modulation at the time of the transit. The observed data give evidence of the envelope in WASP-32b filling the Roche lobe and a comet-like tail of changing geometry and orientation relative to the observer. These changes determine different depths and shapes of the Hα spectral line at the time of transits.
PubDate: 2017-01-01
DOI: 10.1134/s1990341317030087
Issue No: Vol. 72, No. 1 (2017)

• Predictions on the detection of the free-floating planet population with
K2 and spitzer microlensing campaigns
• Authors: L. Hamolli; F. De Paolis; M. Hafizi; A. A. Nucita
Pages: 73 - 80
Abstract: Abstract The K2’s Campaign 9 (K2C9) by the Kepler satellite for microlensing observations towards the Galactic bulge started on April 7, 2016, and is going to last for about three months. It offers the first chance to measure the masses of members of the large population of the isolated dark low-mass objects further away in our Galaxy, free-floating planets (FFPs). Intentionally, this observational period of K2 will overlap with that of the 2016 Spitzer follow-up microlensing project expected to start in June, 2016. Therefore, for the first time it is going to be possible to observe simultaneously the same microlensing events from a ground-based telescope and two satellites. This will help in removing the two-fold degeneracy of the impact parameter and in estimating the FFP mass, provided that the angular Einstein ring radius ΘE is measured. In this paper we calculate the probability that a microlensing event is detectable by two or more telescopes and study how it depends on the mass function index of FFPs and the position of the observers on the orbit.
PubDate: 2017-01-01
DOI: 10.1134/s1990341317030099
Issue No: Vol. 72, No. 1 (2017)

• Wide-field optical monitoring with Mini-MegaTORTORA (MMT-9) multichannel
high temporal resolution telescope
• Authors: G. M. Beskin; S. V. Karpov; A. V. Biryukov; S. F. Bondar; E. A. Ivanov; E. V. Katkova; N. V. Orekhova; A. V. Perkov; V. V. Sasyuk
Pages: 81 - 92
Abstract: Abstract We describe the properties of Mini-MegaTORTORA (MMT-9) nine-channel wide-field optical sky monitoring system with subsecond temporal resolution. This instrument can observe sky areas as large as 900 deg2, perform photometry in three filters close to Johnson BV R system and polarimetry of selected objects or areas with 100–300 deg2 sizes. The limiting magnitude of the system is up to V = 11m for 0.1 s temporal resolution, and reaches V = 15m in minute-long exposures. The system is equipped with a powerful computing facility and dedicated software pipeline allowing it to perform automatic detection, real-time classification, and investigation of transient events of different nature located both in the near- Earth space and at extragalactic distances. The objects routinely detected by MMT-9 include faint meteors and artificial Earth satellites.We discuss astronomical tasks that can be solved using MMT-9, and present the results of the first two years of its operation. In particular, we report the parameters of the optical flare detected on June 25, 2016, which accompanied the gamma-ray burst GRB160625B.
PubDate: 2017-01-01
DOI: 10.1134/s1990341317030105
Issue No: Vol. 72, No. 1 (2017)

sources
• Authors: V. R. Amirkhanyan
Pages: 384 - 394
Abstract: Abstract The relation between the $$D/\sqrt I$$ and I C/I SUM parameters and radiation patterns of the optical and radio components of an extended radio source is analyzed, where D and I are the apparent size and observed radiation intensity, respectively, of the source or its components. The parameters of the pattern in the optical and radio (1.4 GHz) ranges are estimated. The radiation pattern of extended radio-emitting regions is close to spherical and the radiation of the central component is concentrated in a 24◦ wide beam. Its luminosity is a factor of 4.58 higher than that of the extended component of the radio source. The radiation pattern of the optical component of the radio source turned out to be unexpectedly non-spherical: the main lobe of the pattern is about 26◦ wide. The g-band luminosity is 6.4–12.3 times higher than the luminosity of the spherical fraction of the “optical” radiation pattern. A list of 116 new giant radio sources is presented.
PubDate: 2016-10-01
DOI: 10.1134/s1990341316040027
Issue No: Vol. 71, No. 4 (2016)

• Stellar population and evolution of galaxies in groups: the NGC2300 group
• Authors: V. L. Afanasiev; O. K. Silchenko; I. S. Proshina
Pages: 395 - 407
Abstract: Abstract Using panoramic and long-slit spectroscopy at the 6-m telescope of SAO RAS, we studied the stellar population and kinematics of five early-type disc galaxies—members of the NGC2300 group. The evolution of galaxies appears to be absolutely out of synch: while the average age of the stars in the central regions of the galaxies located close to the center of the group ranges from 2 to 7 Gyr, the peripheral spiral galaxies have old nuclei and bulges, with the ages of 10–15 Gyr. The brightest galaxy of the NGC2300 group, which up to now has been considered to be lenticular, of the SA0 type, turned out to be extremely hot dynamically: its bulge rotates slowly, v/σ = 0.06, and the outer parts do not rotate at all.We conclude that the kinematics of the stellar component of NGC2300 indicates that it is not a disc galaxy, but a triaxial spheroid.
PubDate: 2016-10-01
DOI: 10.1134/s1990341316040039
Issue No: Vol. 71, No. 4 (2016)

• FIGGS 2: An HI survey of extremely faint irregular galaxies
• Authors: N. N. Patra; J. N. Chengalur; I. D. Karachentsev; M. E. Sharina
Pages: 408 - 421
Abstract: Abstract We present observations and first results from the FIGGS2 survey. FIGGS2 is an extension of the earlier Faint Irregular Galaxies GMRT survey (FIGGS) towards faint luminosity end. The sample consists of 20 galaxies, 15 of which were detected in HI 21 cm line using the Giant Meterwave Radio Telescope (GMRT). The median blue band magnitude of our sample is approximately −11.m 6, which is more than one magnitude fainter than earlier FIGGS survey. From our GMRT observations we found that, for many of our sample galaxies, the HI disks are offset from their optical disks. The HI diameters of the FIGGS2 galaxies show a tight correlation with their HI mass. The slope of the correlation is 2.08 ± 0.20 similar to what is found for FIGGS galaxies. We also found that for almost all galaxies, the HI disks are larger than the optical disks which is a common trend for dwarf or spiral galaxies. The mean value of the ratio of HI to optical diameter is about 1.54.
PubDate: 2016-10-01
DOI: 10.1134/s1990341316040040
Issue No: Vol. 71, No. 4 (2016)

• SN2015bh in NGC 2770: LBV core collapse in merging of binary system
components
• Authors: V. P. Goranskij; E. A. Barsukova; A. F. Valeev; D. Yu. Tsvetkov; I. M. Volkov; V. G. Metlov; A. V. Zharova
Pages: 422 - 435
Abstract: Abstract We present spectroscopy and multicolor photometry for the optical transient PSN J09093496+3307204 in the galaxy NGC2770, which has afterwards been transferred into the supernova phase and got the name SN2015bh. Medium-resolution spectral observations were carried out between February 2015 to May 2016 using the focal reducer SCORPIO at the 6-m Russian telescope BTA. They were followed by by photometric observations at the BTA and six other telescopes with 0.5–1m apertures. Both at the phase of the SN impostor (2015a) and at the supernova phase (2015b), besides Balmer emissions, the strong Fe II emissions are seen in the spectrum; so, these spectra resemble those of Williams Fe II type classical novae. Taking into account circumstellar, interstellar and galactic absorption, A V = 1.m 14 ±0.m 15), we determined maximum absolute magnitudes of the object to be M V =–15.m 0 ±0.m 3 at the 2015a phase and of M V =–18.m 14 ±0.m 30 at the 2015b phase. The light curve at the 2015b phase is similar to those of SN IIL. The supernova progenitor is a luminous blue variable (LBV) star with the powerful Hα emission. We consider several hypotheses of supernovae explosions following optical transients related with LBV. The hypothesis of core collapse of an evolved massive star interrupting the process of its merging with massive companion in a binary system (a failed luminous red nova) was chosen as the preferable one for this event.
PubDate: 2016-10-01
DOI: 10.1134/s1990341316040052
Issue No: Vol. 71, No. 4 (2016)

• Magnetic stars with wide depressions in the continuum. 1. The Ap star with
strong silicon lines HD5601
• Authors: I. I. Romanyuk; D. O. Kudryavtsev; E. A. Semenko; A. V. Moiseeva
Pages: 447 - 452
Abstract: Abstract Based on observations with the 6-m SAO RAS telescope, we have found that chemically peculiar star with a large depression of the continuum at λ5200 Å and strengthened silicon lines in the spectrum has a strong magnetic field. The longitudinal field component B e has a negative polarity and varies from −300 G to −2000 G with a period of 1.756 days. Photometric variations of brightness take place with the same period. We determined the variability of the radial velocity at times of about tens of years pointing to a possible binarity of the object. We have built a magnetic model of this star, determined the inclination angles of the rotation axis to the line of sight i = 20° and of the dipole axis to the rotation axis β = 116°, and the field strength at the pole is B p = 10 kG. We carried out a chemical composition analysis and found a lack of helium for almost an order of magnitude, some overabundance of silicon and metal elements for more than an order of magnitude, particularly, cobalt for three orders of magnitude.
PubDate: 2016-10-01
DOI: 10.1134/s1990341316040076
Issue No: Vol. 71, No. 4 (2016)

• Features of magnetic field structures in chemically peculiar stars. IV
• Authors: Yu. V. Glagolevskij; A. F. Nazarenko
Pages: 453 - 462
Abstract: Abstract We present results of modeling of the sample of magnetic stars. We have obtained such important for magnetic star physics parameters as the mean surface magnetic field B s , the magnetic field at magnetic poles—B p , the dipole inclination to the rotation equatorial plane α, and the distance to monopoles from the center of the star Δa. We present some information onmagnetic star physics that helps to understand the derived results better.
PubDate: 2016-10-01
DOI: 10.1134/s1990341316040088
Issue No: Vol. 71, No. 4 (2016)

• On the formation of TW Crv optical radiation
• Authors: V. V. Shimansky; A. A. Mitrofanova; N. V. Borisov; S. N. Fabrika; A. I. Galeev
Pages: 463 - 474
Abstract: Abstract We present the analysis of the optical radiation of the young pre-cataclysmic variable TW Crv. Spectroscopic and photometric observations were obtained at the SAO RAS 6-m BTA telescope and at the Russian-Turkish RTT-150 telescope. The light curves of the system posses nearly sinusoidal shapes with the amplitudes of Δ m > 0.m7, what is typical for young pre-cataclysmic variables with sdO-subdwarfs and orbit inclinations of less than 45◦. The optical spectrum contains dominant radiation of the hot subdwarf with the HI and He II absorption lines and strong emission lines, which are formed in the atmosphere of the secondary owing to the reflection effects. Radial velocities of the cool star were measured by analyzing the λλ 4630–4650 Å Bowen blend, which for the first time allowed to determine the component masses. A numerical simulation of the light curves and spectra of TW Crv, obtaining a complete set of systems fundamental parameters was carried out. The hot star parameters prompt its belonging to the sdOsubdwarf class at the stage of transition to the cooling white dwarf sequence. The absence of its observable planetary nebula is caused by a long-lasting evolution of the system after the common envelope state. The secondary component has a luminosity excess, which is typical for other young sdO-subdwarf precataclysmic variables. Its position on the “age−−luminosity excess” diagram points at the accuracy of the obtained set of TW Crv fundamental parameters and at the similarity of its evolutionary and physical conditions with that of other BE UMa-type objects.
PubDate: 2016-10-01
DOI: 10.1134/s199034131604009x
Issue No: Vol. 71, No. 4 (2016)

• Detection of circular polarization and low-amplitude photometric
variability of the white dwarf WD1748+508
• Authors: K. A. Antonyuk; S. V. Kolesnikov; N. V. Pit; G. G. Valyavin; A. F. Valeev; T. E. Burlakova; G. A. Galazutdinov
Pages: 475 - 478
Abstract: Abstract We report the results of a polarimetric and photometric study of the cool white dwarf WD1748+508. Observations were performed during four consecutive nights on the telescopes of the Crimean Astrophysical Observatory. As a result, polarization was detected in the V band at the level of −0.36 ± 0.087% and the star was found to be photometrically variable with a period ranging from five hours to about two days. Throughout the entire observing set the variability amplitude was constant and equal to about 10 ± 1 mmag. Non-zero circular polarization directly indicates that the white dwarf has a global magnetic field with a strength of 10 MG or higher.We interpret the photometric variations found in this study in terms of rotationally modulated variability of magnetic properties of the star’s atmosphere.
PubDate: 2016-10-01
DOI: 10.1134/s1990341316040106
Issue No: Vol. 71, No. 4 (2016)

• ADAM low- and medium-resolution spectrograph for 1.6-m AZT-33IK telescope
• Authors: V. L. Afanasiev; S. N. Dodonov; V. R. Amirkhanyan; A. V. Moiseev
Pages: 479 - 488
Abstract: Abstract We describe the design of a suspended low- and medium-resolution spectrograph (R ≈ 300–1300) designed and made at the Special Astrophysical Observatory of the Russian Academy of Sciences for the 1.6-m AZT-33IK telescope of Sayan Observatory of the Institute of Solar-Terrestrial Physics of the Siberian Branch of the Russian Academy of Sciences. We report the results of laboratory measurements of the parameters of the instrument and tests performed on the 1-m Zeiss-1000 telescope of the Special Astrophysical Observatory of the Russian Academy of Sciences. We measured the total quantum efficiency of the “spectrograph + telescope + detector” system on AZT-33IK telescope, which at its maximum reaches 56%. Such a hight transparency of the spectrograph allows it to be used with the 1.6-m telescope to determine the types and redshifts of objects with integrated magnitudes m AB ≈ 20–21, and this result was confirmed by actual observations.
PubDate: 2016-10-01
DOI: 10.1134/s1990341316040118
Issue No: Vol. 71, No. 4 (2016)

• Dichroic circular polarization analyzer for the Main Stellar Spectrograph
of the 6-m telescope
• Authors: G. A. Chountonov
Pages: 489 - 495
Abstract: Abstract We describe a dichroic circular polarization analyzer with a double image slicer providing seven slices for each polarization developed for the Main Stellar Spectrograph of the 6-m telescope of the Special Astrophysical Observatory of the Russian Academy of Sciences. The analyzer is designed for measuring stellar magnetic fields using the Zeeman effect and represents an upgraded version compared to earlier used polarization analyzers. We report the parameters of the analyzer and estimate the accuracy of measurements performed with it.
PubDate: 2016-10-01
DOI: 10.1134/s199034131604012x
Issue No: Vol. 71, No. 4 (2016)

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