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501. AFKwin.html: Alexander Kholtygin (Russian Home Page)
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Ссылки http://www.astro.spbu.ru/staff/afk/indexW.html -- 1.3 Кб -- 19.11.2010
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502. http://www.astro.spbu.ru/staff/afk/Papers/2007/Fourier2007E.pdf
... SEARCH FOR HARMONIC COMPONENTS OF TIME SERIES WITH VERY LARGE GAPS A. F. Kholtygin,1, A. B. Shneiwais,1 T. E. Burlakova,2 and Yu. ... The results of this analysis are used to search for harmonic components in the variation of the H line profile in spectra of the triple star Ori A obtained in 2004 with the BTA telescope at the Special Astrophysical Observatory of the Russian Academy of Sciences. Keywords: time series: Fourier analysis: hot stars: line profiles: variability 1. ... Short time series. ...
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Ссылки http://www.astro.spbu.ru/staff/afk/Papers/2007/Fourier2007E.pdf -- 166.3 Кб -- 19.11.2010
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503. Kholtygin et al., "Stochastic Data in Astronomy. II.", Astrophysics (2007)
Kholtygin A.F., Shneiwais A.B., Burlakova T.E., Milanova Yu.V. Stochastic Data in Astronomy. ... Fourier Analasis of Strongly Unevaen Time Series . Astrophysics, 50 , 225-2387 ( 2007 ) Original Russian Text published in Zhurnal Astrofizika , 50 , pp. 281-297 ( 2007 ) . ... It is supposed that analysed time series consist of harmonic components with amplitude $A$ and a period larger than the longest segment of the time series and the noise component with variance $N^2$. ...
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Ссылки http://www.astro.spbu.ru/staff/afk/Papers/2007/Fourier2007abstr.html -- 2.8 Кб -- 19.11.2010
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504. http://www.astro.spbu.ru/staff/afk/Papers/2007/RhoLeo2007MF.pdf
Physics of Magnetic Stars, 2007, pp. 262-270 Line profile variability and the possible magnetic field in the spectra of supergiant Leo A.F. Kholtygin1 , G.A. Chountonov2 , S.N. Fabrika2 , T.E. Burlakova Kang Dong-il3 , G.A. Galazutdinov2,4 , M.V. Yushkin2 1 2 2,3 ... Astronomy and Space Science Institute, Optical Astronomy Division, 61-1, Whaam-Dong, YuseongGu, Daejeon, 305-348, Korea 1 Intro duction Line profiles in sp ectra of OB stars are usually strongly variable (Morel et al ...
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Ссылки http://www.astro.spbu.ru/staff/afk/Papers/2007/RhoLeo2007MF.pdf -- 256.6 Кб -- 19.11.2010
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505. Kholtygin et al., "rho Leo", AZh (2007)
Kholtygin A.F., Fabrika S.N., Burlakova T.E., Valyavin G.G., Chuntonov G.A., Kudryavtsev D.O., Kang Dong-il, Yushkin M.V., Galazutdinov G.A. Microvariability of Line Profiles in the Spectra of OB stars III. Supergiant rho Leo . Astronomy Reports, 51 , 920-931 ( 2007 ) . ... 1016-1028 ( 2007 ) . ... We detected variability in the HeI, SiII, SiIII, and NII line profiles, which may be due to rotational modulation of the profiles and photospheric pulsations of $\rho\,$Leo. ...
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Ссылки http://www.astro.spbu.ru/staff/afk/Papers/2007/rhoLeo2007abstr.html -- 2.5 Кб -- 19.11.2010
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506. Kholtygin et al., Magn. Field Conf., August 2006 (2007)
Kholtygin A., Chountonov G.A., Fabrika S.N., Burlakova T.E., Valyavin G.G., Kang Dong-il, Galazutdinov G.A., Yushkin M.V. Line profile variability in the spectra of supergiant rho Leo and the possible magnetic field . ... Conference, held in the Special Astrophysical Observatory of the Russian AS, August 28 - September 1, 2006, Eds.: Yu. ... Rsults of a study of fast line profile variability (lpv) in spectra of bright B1 supergiant rho Leo and searching is magnetic field are reported. ...
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Ссылки http://www.astro.spbu.ru/staff/afk/Papers/2007/rhoLeo2007MFabstr.html -- 2.2 Кб -- 19.11.2010
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507. http://www.astro.spbu.ru/staff/afk/Papers/2007/Fourier2007R.pdf
... 0.5 -1 A | ... ЕИ N = 160 A/N = 5 ИД бв К T = = 2.1 -1 ЕК Н nu 10 8 6 4 2 0 0 nu 10 8 6 4 2 0 0 nu 10 8 6 4 2 0 0 nu 10 8 6 4 2 0 0 nu 10 8 6 4 2 0 0 nu 10 ... 6 fi 1 2 3 4 5 6 fi 1 2 3 4 5 6 fi 1 2 3 4 5 6 fi 1 2 3 4 5 6 fi 1 2 3 4 5 6 fi 1 2 3 4 5 6 fi 1 2 3 4 5 6 fi 1 2 3 4 5 6 fi К 160 + 160 T д =3 К И -7 Д A/N = 5 ЕИ Д К К T = 0.003 d q = 10 N = 40 + 40 Tд Е Д Е? N = 80 + 80 И N= Н T T T 2.5 2.5 2.5 2 2 2 1.5 1.5 1.5 1 1 1 0.5 0.5 0.5 0 V - 300 - 200 - ...
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Ссылки http://www.astro.spbu.ru/staff/afk/Papers/2007/Fourier2007R.pdf -- 605.6 Кб -- 19.11.2010
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508. Kholtygin A.F. Non-Radial Pulsations., (2007)
Kholtygin A.F. Non-radial pulsations of early-type stars (in russian) in Methods of spectroscopy in thew modern Astrophysics , Proc. of the Conference, held in Institiute of Astronomy, September 13-15, 2006, Moscow, Eds: L.I.Mashonkina, M.E.Sachkov, pp. 316-335 (2007) . Nonradial pulsations in early spectral class stars. The results of the searching and analysis of the microvariability of the line proТle in spectra of bright OB-stars are presented. ...
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Ссылки http://www.astro.spbu.ru/staff/afk/Papers/2007/NRP2007abstr.html -- 2.4 Кб -- 19.11.2010
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509. http://www.astro.spbu.ru/staff/afk/Papers/2008/Kholtygin2008NeTediagnE.pdf
... Ultimately, he derived a formula relating the temperature of the gas in nebulae to the intensity ratio of forbidden lines observed in their spectra. The method of determining the temperatures of nebulae from the intensity ratios of forbidden lines in their spectra was proposed on the basis of these studies. ... 13) This ratio has a very weak temperature dependence. ... The electron temperatures of a large number of nebulae have been determined from the intensity ratios of forbidden lines. ...
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Ссылки http://www.astro.spbu.ru/staff/afk/Papers/2008/Kholtygin2008NeTediagnE.pdf -- 157.1 Кб -- 19.11.2010
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510. http://www.astro.spbu.ru/staff/afk/Papers/2008/Kholtygin2008NeTediagnR.pdf
... k И A21 ?К?К ? ... К К? ДК К НИ ДЕ Е (A21 + n q21 + n q23 )n2 , n q12 n1 +(A32 + n q32 )n3 = = (A31 + A32 + n (q31 + q32 )) n3 . n q13 n1 + n q23 n2 n q 12 (A31 + A n2 = n 1 (A21 + n q21 )(A31 n q12 n n3 = n 1 (A21 + n q21 )(A31 +n + A32 q23 + + A32 q 31 + n q32 )+ n q 13 (A32 + n q 32 ) + n q31 + ne q32 )+ n q23 (A31 + n q31 n q13 (A21 + n q21 + n q23 ) + n q31 + ne q32 )+ n q23 (A31 + n q31 Й Й Й ДЕ 32 ) ) , . ... И Eki Iki И И Р К 21 k iИ Й ПКОК ДЕ И I21 E21 12 = = I32 E32 23 1+ q12 q13 . ...
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Ссылки http://www.astro.spbu.ru/staff/afk/Papers/2008/Kholtygin2008NeTediagnR.pdf -- 936.7 Кб -- 19.11.2010
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511. Yu.V. Milanova, A.F. Kholtygin, He, C, N, and O Abundances in an Ensemble of
Yu.V. Milanova, A.F. Kholtygin, . UV lines in spectra of Planetary Nebulae(in russian) in Proc. of the Conference, held in Institiute of Astronomy, May 19-20, 2008, Moscow, Ultravililet Universe II , Eds: , B.M.Shustov, M.E.Sachkov, E.A.Kilpio , M., Yanus-K, pp. 208-212 ( 2008 ) . The modern observations of planetary nebulae (PNe) are used to create a new catalogue of element abundances for galactic and extragalactic PNe. Some of these abundances, especially C ones, need to be refined. ...
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Ссылки http://www.astro.spbu.ru/staff/afk/Papers/2008/MilanovaKholtygin2008abstr.html -- 2.2 Кб -- 19.11.2010
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512. Yu.V. Milanova, A.F. Kholtygin, He, C, N, and O Abundances in an Ensemble of
A.F. Kholtygin, . Plasma Diagnostics of Planetary Nebulae (in russian) Astrophysics , 51 , 363-383 ( 2008 ) . Diagnostics for the rarefied plasmas in gaseous nebulae are reviewed, beginning with the pioneering papers of V. A. Ambartsumian. These papers, as well as the diagnostic techniques which have been developed on the basis of ideas contained in them, are discussed. Diagnostic techniques for homogeneous, as well as inhomogeneous, plasmas are described
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Ссылки http://www.astro.spbu.ru/staff/afk/Papers/2008/Kholtygin2008NeTediagnAbstr.html -- 1.9 Кб -- 19.11.2010
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513. http://www.astro.spbu.ru/staff/afk/Papers/2008/MilanovaKholtygin_UVuniR.pdf
... К И И ДЕ К И Й Й И ?Й К Abstract The modern observations of planetary nebulae (PNe) are used to create a new catalogue of element abundances for galactic and extragalactic PNe. Some of these abundances, esp ecially C ones, need to b e refined. ... К 18 7 6 5 4 3 2 1 0 16 14 Density (PDF) РЫЬК Й Й Й Й Density (PDF) 12 10 8 6 4 2 8.3 8.4 8.5 lg(N/H)+12 8.6 8.7 0 8.85 8.9 8.95 9 lg(O/H)+12 9.05 9.1 К ОК ЕИ Ц И МО И И И Д К Й ОМЙПМБК НМБИ Д К ОЕК К Й ПК Д И ? ...
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Ссылки http://www.astro.spbu.ru/staff/afk/Papers/2008/MilanovaKholtygin_UVuniR.pdf -- 289.4 Кб -- 19.11.2010
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514. http://www.astro.spbu.ru/staff/afk/Papers/2009/MilanovaKholtygin2009E.pdf
... 35, No. 8, pp. 563ґ573. i He, C, N, and O Abundances in an Ensemble of Galactic Planetary Nebulae Yu. ... Taking into account the inaccuracies in the corrections for the ionization stages of the elements whose lines are absent in the PNe spectra increases the errors in the He abundance to 0.1 dex and in the C, N, and O abundances to 0.2ґ0.3 dex. ... To ascertain which PNe belonging to the Galactic disk are similar to bulge objects, we compared the He, C, N, and O abundances in bulge and disk nebulae...
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Ссылки http://www.astro.spbu.ru/staff/afk/Papers/2009/MilanovaKholtygin2009E.pdf -- 791.2 Кб -- 19.11.2010
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515. Yu.V. Milanova, A.F. Kholtygin, He, C, N, and O Abundances in an Ensemble of
Yu.V. Milanova, A.F. Kholtygin . He, C, N, and O Abundances in an Ensemble of Galactic PNe (in russian) Astronomy Letters,, 35 , 518-533 ( 2006 ) Original Russian Text are published in Pis'ma v Astronomicheskii Zhurnal , 35 , No. 8, pp. 563-573 ( 2009 ) . ... The He abundance is determined with an accuracy of 0.06 dex, while the errors in the C, N, and O abundances are 0.1-0.2 dex. ... The elemental abundances in PNe of various Galactic subsystems and the Magellanic Clouds have been analyzed. ...
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Ссылки http://www.astro.spbu.ru/staff/afk/Papers/2009/MilanovaKholtygin2009abstr.html -- 3.2 Кб -- 19.11.2010
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516. http://www.astro.spbu.ru/staff/afk/Papers/1998/InhomPNe1998.pdf
... We reconsider the problem of the difference between the abundances of carbon and oxygen in galactic planetary nebulae (PN) derived from the intensities of the recombination and collisionally excited lines. ... The formulae for calculation of the nebular line intensities in presence of both temperature and density fluctuations are given. ... C and O abundances We have fitted the line intensities for more than 70 PNe including all of those which were considered by RS except NGC 2242, IC 418 and M1-14....
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Ссылки http://www.astro.spbu.ru/staff/afk/Papers/1998/InhomPNe1998.pdf -- 434.1 Кб -- 19.11.2010
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517. Kholtygin, AA, V. 329 (1998)
... We reconsider the problem of the difference between the abundances of carbon and oxygen in galactic planetary nebulae (PN) derived from the intensities of the recombination and collisionally excited lines. ... The intensities of the forbidden [OIII] lines, the CII, CIII and CIV recombination lines and the CIII]$\,\lambda\,$1909 UV intercombination doublet for different values of the mean electron temperature $T_0$ in PNe and the {\em rms} temperature variation $\mbox{\bm $t^2$}$, are calculated. ...
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Ссылки http://www.astro.spbu.ru/staff/afk/Papers/1998/InhomPNe1998abstr.html -- 3.2 Кб -- 19.11.2010
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518. http://www.astro.spbu.ru/staff/afk/Papers/2000/EmUnHomPl2000.pdf
... О Й ИЦ ЧД И ki Й n = n(X ) Й К Eki = Eki = h ki V ЕИ Й И Й И + И Й ДНЕ К? К И eff rki eff n rki dV . ... Eki /Emn И ? И И И И eff rki К? СССЙЮИ ЦСССЙСЮ ЧСССИ К eff rki (T0 ,n0 )И e Й И К Й Й Й Й 0 eff Eki Eki = hki rki (T0 ,n0 ) e V eff hki rki (T0 ,n0 ) N , e n dV = N Й Н И X К? T0 = V T0 Te ne n dV / V Н ИН ne n dV . ... E 0 И Е= Te = To eff 1 2 rki eff -1 2 (rki ) Te 2 2 Te Te =To ДЕ t 2 К ? ... зижгд нзКИ К ИПИН К И К П И Н ОК ИИ И П НИ Н К НМ НН НО НП Н Н Н Н Н Н ОМ ОН ООК КК ИК ? ...
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Ссылки http://www.astro.spbu.ru/staff/afk/Papers/2000/EmUnHomPl2000.pdf -- 364.9 Кб -- 19.11.2010
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519. Kholtygin, Astrophysics (2000)
A.F.Kholtygin . Emission of the inhomogeneous plasma: line intensities and element abundances in the gaseous nebulae with T e and n e fluctuations, Astrophysics , 43 , 627-640 (2002) . ... We calculate radial and vertical abundance gradients of C, N, O, Ne, Ar, Cl and S depending of different ages of the central star of the nebula. It have been founded statistically significant dependence of abundance gradients with the age of central star. ...
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Ссылки http://www.astro.spbu.ru/staff/afk/Papers/2000/EmUnHomPl2000abstr.html -- 2.3 Кб -- 19.11.2010
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520. Broawn et al., MN, V. 352 (2004)
Brown J.C., Telfer D., Li Q., Hanuschik R., Cassinelli J. P., Kholtygin A. The effect of rotational gravity darkening on magnetically torqued Be star discs . ... 1 is not the optimum for creation of hot star discs which, in terms of emission measure for example, is found to occur in a broad peak around So~ 0.5-0.6 depending slightly on the wind velocity law. The relationship of this analytic quasi-steady parametric MTD model to other work on magnetically guided winds is discussed. ...
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Ссылки http://www.astro.spbu.ru/staff/afk/Papers/2004/MTD2abstr.html -- 3.0 Кб -- 19.11.2010
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