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9121. Answers and comments to the exercises
... Also note that with fix form text in positions 73 to 80 was considered to be a comment. ... PROGRAM TEST_ADAPTIVE_QUAD IMPLICIT NONE INTERFACE FUNCTION F(X) RESULT ( FUNCTION _VALUE) REAL , INTENT (IN) :: X REAL :: FUNCTION _VALUE END FUNCTION F END INTERFACE INTERFACE RECURSIVE FUNCTION ADAPTIVE_QUAD (F, A, B, TOL, ABS_ ERROR ) RESULT ( RESULT ) REAL , EXTERNAL :: F REAL , INTENT (IN) :: A, B, TOL REAL , INTENT (OUT) :: ABS_ ERROR REAL :: RESULT ...
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Ссылки http://star.arm.ac.uk/f77to90/answers.html -- 28.1 Кб -- 12.06.1996
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9122. Intrinsic functions in Fortran 90
... Array functions . ... Random number routines There is a large a number of intrinsic functions and five intrinsic subroutines in Fortran 90. ... ALL(MASK, dim) returns a logical value that indicates whether all relations in MASK are .TRUE. , along only the desired dimension if the second argument is given. ... SIZE(ARRAY, dim) is a function which returns the number of elements in an array ARRAY , if DIM is not given, and the number of elements in the relevant dimension if DIM is included. ...
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Ссылки http://star.arm.ac.uk/f77to90/a5.html -- 46.1 Кб -- 12.06.1996
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9123. http://star.arm.ac.uk/~ambn/yzcmi83_final.ps
A&A manuscript no. (will be inserted by hand later) Your thesaurus codes are: 07 (08.01.2; 08.01.3; 08.06.1; 08.12.1; 08.09.2 YZ CMi) ASTRONOMY AND ASTROPHYSICS 6.11.1995 Flare energetics: Analysis of a large flare on YZ CMi observed simultaneously in the ultraviolet, optical and radio ? ... Analysis of a large flare on YZ CMi 11 E opt ъ 2 10 32 erg, the total energy losses in the Uґband, the beam flux becomes a simple function of the optical flare area F b = 4 10 8 ь \Gamma1 opt . ...
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Ссылки http://star.arm.ac.uk/~ambn/yzcmi83_final.ps -- 626.6 Кб -- 31.05.1996
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9124. http://star.arm.ac.uk/~ambn/prom.ps
PROMINENCES ON LATE TYPE ACTIVE STARS P.B. BYRNE Armagh Observatory Armagh BT61 9DG, N. Ireland Abstract. ... Introduction The solar paradigm is widely used to explain a broad range of phenomena on lateґtype stars. ... These features cannot be at the stellar photosphere, since they would cross the rotationally broadened profile in a time P rot /2 and so Cameron & Robinson interpreted them as clouds of neutral hydroґ gen supported high above the photosphere in a manner reminiscent of solar prominences. ...
9125. http://star.arm.ac.uk/~ambn/preprint.ps
by hand later) Your thesaurus codes are: 08(02.1,02.4,11.1,18.1),03.20.7 ASTRONOMY AND ASTROPHYSICS 7.3.1995 Crossґcorrelation radial velocity measurements of chromospherically active binaries A. G. Gunn 1 , J. C. Hall 2 , G. W. Lockwood 2 , and J. G. Doyle 1 1 Armagh Observatory ... , N. Ireland 2 Lowell Observatory, 1400 Mars Hill Road, Flagstaff, Arizona 86001, USA February 1995 Main Journal Running title: Radial velocity measurements of active binaries Abstract ...
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Ссылки http://star.arm.ac.uk/~ambn/preprint.ps -- 892.3 Кб -- 31.05.1996
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9126. http://star.arm.ac.uk/~ambn/mzbpap.ps
... Basically, though 34 these additional modifications were initialized by study CP stellar spectra, they have quite general applications. ffl chemical elements up to Z = 82 + ffl vertical stratification of stellar atmosphere ґ chemical elements + ffl iterative abundance process + ffl horizontal stratification + ffl partition function option (Mn and Ga species) + There is no reason for the cutoff of chemical species at Z=82. ... Figure 2 illustrates vertical stratification of helium. ...
9127. http://star.arm.ac.uk/~ambn/pcuvflare.dvi-ps
... 2 Flares on dMe stars 2.1 dMe quiescent emission Quiescent emission from dMe flare stars is characterised by strong line emisґ sion from neutral and ionised atomic species arising in temperatures characґ teristic of the solar chromosphere (6 10 3o K?T e ?10 4o K) and transition region (3 10 4o K?T e ?2 10 5o K). ... 4 Byrne & McKay, 1990 2.2 dMe flaring emission During flares all of the lines visible in the quiescent spectrum are seen to inґ crease, some by factors of up to ?10 or greater. ...
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Ссылки http://star.arm.ac.uk/~ambn/pcuvflare.dvi-ps -- 318.1 Кб -- 31.05.1996
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9128. http://star.arm.ac.uk/~ambn/hkaat91.ps
... 980+0.4307E. Date JD Phase Exp Date JD Phase Exp Date JD Phase Exp 2448490+ (sec) 2448490+ (sec) 2448490+ (sec) 24/8 2.9399 0.637 300 25/8 3.9370 0.952 300 26/8 4.9321 0.263 300 2.9602 0.684 300 3.9569 0.998 300 4.9680 0.346 300 2.9801 0.730 300 3.9894 0.074 300 4.9959 0.411 300 3.0000 0.777 300 3.9974 0.092 300 5.0238 0.475 300 3.0040 0.786 300 4.0412 0.194 300 5.3085 0.137 300 3.0319 0.851 ... Young et al. (1990) discovered a unique behaviour of HK Aqr's Hff emission....
9129. http://star.arm.ac.uk/~ambn/iau176rev.ps
ON THE BELIEVABILITY OF POLAR SPOTS P. BRENDAN BYRNE Armagh Observatory College Hill, Armagh BT61 9DG, N. Ireland Abstract. Polar spots in Doppler Imaging maps of rapidly rotating lateґ type stars, especially the active components of RSCVn binaries, represent a major break with the solar paradigm, within which spots are only found at low latitudes. ... Introduction The technique of Doppler Imaging offers the potential to resolve in some detail spot distributions on active lateґtype stars. ...
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Ссылки http://star.arm.ac.uk/~ambn/iau176rev.ps -- 140.6 Кб -- 31.05.1996
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9130. http://star.arm.ac.uk/~ambn/euve_mm1.ps
manuscript no. (will be inserted by hand later) Your thesaurus codes are: 07 (08.01.1; 08.01.2; 08.03.5; 08.06.1; 08.09.2 EUVEJ2056ґ 17.1 ; 08.12.1) ASTRONOMY AND ASTROPHYSICS 15.5.1995 Optical identification of EUV sources: The secrets of EUVE J2056 ґ 17.1 M. Mathioudakis 1 , J.J. Drake 1 , N. Craig 1 , D. Kilkenny 2 , J.G. Doyle 3 , M.M. Sirk 1 , J. Dupuis 1 , A. Fruscione 1 , C.A ... 1994). ... The flare on EUVE J2056ґ17.1 is one of the most enґ ergetic flares reported on a lateґtype dwarf. ...
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Ссылки http://star.arm.ac.uk/~ambn/euve_mm1.ps -- 1447.6 Кб -- 31.05.1996
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9131. http://star.arm.ac.uk/~ambn/genflare.dvi-ps
Flares, the solarґstellar connection P. Brendan Byrne 1 Armagh Observatory, Armagh BT61 9DG, N. Ireland 2 eMail: pbb@star.arm.ac.uk 1 Introduction The systematic study of stellar flares in now more than 30 years old. ... 1.1 In which stars do we find stellar flares? ... 2 Comparison between dMe and solar flares 2.1 Optical Optical spectroscopy of fast stellar flares shows that the rise and initial decay is dominated by broadґband continuum and highґexcitation emission in such lines as HeI and HeII. ...
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Ссылки http://star.arm.ac.uk/~ambn/genflare.dvi-ps -- 165.9 Кб -- 31.05.1996
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9132. http://star.arm.ac.uk/~ambn/euve_counts_rate.ps
... SOURCE NAME Dist. log NH fCIV Lex /B Al/Ti/C (Index) Common or HD (pc) (cm \Gamma2 ) (10 \Gamma13 ) ct ks \Gamma1 oe f 6:8 ct ks \Gamma1 oe f 6:8 003 HD 3196 21 18.79 2.8 36\Sigma11 5 1.2 59\Sigma20 4 6.3 004 i And 31 19.81 18.1 37 \ Sigma 5 10 7.2 16 \ Sigma 5 3 11.8 005 CF Tuc 54 19.84 4.2 67 \ Sigma 12 8 14.4 30 UL ґ 22.9 006 UV Psc + 125 19.09 ґ 19 \ Sigma 7 3 0.8 56 UL ґ 21.7 008 HD 8358 60 18.73 1.4 33 \ ... DR Dra has 20% higher EUVE counts. ... EUV Emission from RS CVn binaries Fig. ...
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Ссылки http://star.arm.ac.uk/~ambn/euve_counts_rate.ps -- 489.7 Кб -- 31.05.1996
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9133. http://star.arm.ac.uk/~ambn/acl_paper_I.ps
A&A manuscript no. (will be inserted by hand later) Your thesaurus codes are: 08 (08.01.3; 08.03.4; 08.12.1; 02.18.7; 02.12.3) ASTRONOMY AND ASTROPHYSICS 5.12.1994 The upper chromosphere and lower transition region of dMe stars. ... Models for the upper chromosphere and the lower transition region of dM0eґdM2e stars are presented. ... The analysis of the Hff profile in the dM1e star V1005Ori (=Gl 182) indicates that the temperature gradient in the lower transition region is smaller than solar. ...
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Ссылки http://star.arm.ac.uk/~ambn/acl_paper_I.ps -- 377.5 Кб -- 31.05.1996
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9134. http://star.arm.ac.uk/~ambn/acl_paper_II.ps
A&A manuscript no. (will be inserted by hand later) Your thesaurus codes are: 08 (08.01.3; 08.03.4; 08.12.1; 02.12.1) ASTRONOMY AND ASTROPHYSICS 30.1.1995 Helium lines in lateґtype dwarfs. A. C. Lanzafame ? ... The vaґ lidity of the weakly nonґuniform approximation for dMe stars established in Lanzafame (1994a) for the lower transition region of dMe stars implies that streaming particles have virtually no role in the formation of the lines. ... Helium lines in lateґtype dwarfs. ...
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Ссылки http://star.arm.ac.uk/~ambn/acl_paper_II.ps -- 613.1 Кб -- 31.05.1996
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9135. http://star.arm.ac.uk/~ambn/abstract173.html
In this new series we present observations and modelling of spectral lines formed in main sequence star chromospheres (from G0 to M8). in this paper, we discuss the Hydrogen line formations in very active dMe stellar chromospheres. ... Our final model atmosphere is described in the next paper in this series. ... We found that observations are best reproduced by a chromospheric structure including a constant temperature gradient (in a log(M) scale) in the chromosphere and transition region. ...
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Ссылки http://star.arm.ac.uk/~ambn/abstract173.html -- 3.5 Кб -- 31.05.1996
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9136. http://star.arm.ac.uk/~ambn/abstract174.html
... We give evidence that lower pressure model chromospheres can alos reproduce the Balmer line profiles, but give Lyman surface fluxes overestimated by more than an order of magnitude. ... We obtain the Paschen lines in emission and Paschen decrements as large as 41 for Pa$_{\beta}$. ... Formation of all Hydrogen series is collisionally controlled and takes place in a rather thin layer at the top of the chromosphere (Balmer, Paschen, and Brackett) or in the transition region (Lyman). ...
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Ссылки http://star.arm.ac.uk/~ambn/abstract174.html -- 4.8 Кб -- 31.05.1996
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9137. http://star.arm.ac.uk/~ambn/abstract175.html
Ultraviolet and optical data are used to look at surface inhomogeneities on the active close binary system SZ Piscium. Lower chromospheric emission lines such as Mg II h\ , and to the lesser extend the upper chromospheric/lower transition region lines of O I 1305 $\AA$ and C II 1335$\AA$ show a pronounced decrease when the F star is eclipsing the K sub-giant. However, higher temperature lines such as the resonance line of C IV 1559$\AA$ do not show any change in flux. ...
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Ссылки http://star.arm.ac.uk/~ambn/abstract175.html -- 1.9 Кб -- 31.05.1996
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9138. http://star.arm.ac.uk/~ambn/abstract176.html
Recent observational results by Mathioudakis et al. (1992) have suggested that optical U-band flares are a frequent occurrance on the RS CVn star, II Peg. ... We show that these data are inconsistent with the flaring rates reported earlier and suggest that either II Peg was in a state of low flare activity in 1992, or that it was unusually active at the time of Mathioudakis et al's observations. Key words: Stars - late-type; stars - RS CVn; activity; flares; II Peg ...
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Ссылки http://star.arm.ac.uk/~ambn/abstract176.html -- 1.6 Кб -- 31.05.1996
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9139. http://star.arm.ac.uk/~ambn/abstract177.html
The variations of the orbital period of the RS CVn-type binary system SZ Psc are examined through a detailed description of the O-C diagram and the use of a new analysis technique. Continuous changes of very large magnidude have been found. ... A combination of a magnetic activity cycle mechanism and an enhanced stellar wind are found to reproduce satisfactorily the period changes. Key words: orbital period variations - mass transfer - mass loss - third body - magnetic activity ...
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Ссылки http://star.arm.ac.uk/~ambn/abstract177.html -- 1.8 Кб -- 31.05.1996
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9140. http://star.arm.ac.uk/~ambn/abstract178.html
Magnetic activity gives rise to a number of variable phenomena in premain sequence stars, main sequence stars and binary systems for instance. Notably, flares and hot and dense outer atmospheres are most commonly observed. We need to investigate theoretically the possible spectral signatures of chromospheres so as to interpret the remarkable variety of observations, and discriminate the chromospheric counterpart to other possible contributions, such as cool coronal loops. ...
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Ссылки http://star.arm.ac.uk/~ambn/abstract178.html -- 1.6 Кб -- 31.05.1996
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