Time-resolved high-resolution CCD spectroscopy covering two 4.6-hr orbits of DQ Her are presented. Analysis of the Na I 8183,8195 A absorption doublet yields estimates of the secondary star's projected orbital velocity and rotational broadening. The estimate of the projected orbital velocity is refined using models of the effects of irradiation on the secondary star, producing a final value of 227 +/- 10 km/s. The stellar masses are estimated at M1 = 0.60 +/- 0.07 and M2 = 0.40 +/- 0.05 solar mass.
{"title":"On the mass of nova DQ Hercules (1934)","authors":"K. Horne, W. Welsh, R. Wade","doi":"10.1086/172752","DOIUrl":"https://doi.org/10.1086/172752","url":null,"abstract":"Time-resolved high-resolution CCD spectroscopy covering two 4.6-hr orbits of DQ Her are presented. Analysis of the Na I 8183,8195 A absorption doublet yields estimates of the secondary star's projected orbital velocity and rotational broadening. The estimate of the projected orbital velocity is refined using models of the effects of irradiation on the secondary star, producing a final value of 227 +/- 10 km/s. The stellar masses are estimated at M1 = 0.60 +/- 0.07 and M2 = 0.40 +/- 0.05 solar mass.","PeriodicalId":9423,"journal":{"name":"Bulletin of the American Astronomical Society","volume":"23 12 1","pages":"738"},"PeriodicalIF":0.0,"publicationDate":"1993-06-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"85019342","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
This paper reports on the computations necessary to place the FK5 Extension (epoch of place B1950.0) on the B1950.0/FK4 system from its published form and the availability of this version of the catalog. An application of the utility of the new version of the FK5 Extension, to the AGK3U, is given too. This confirms both the system of the AGK3U and the estimated values of its equatorial coordinate and proper motion mean errors. In addition, we have fully exploited the flexibility of the method of infinitely overlapping circles to compute a mean epoch of place/FK4 version of the FK5 Extension which we also make available. These modifications include taking into account the changes induced by the new system of general precession constants, adjusting for the e-terms of aberration, correcting for both the FK5/FK4 equinox offset and motion, and the FK5/FK4 positional and the proper motion systematic differences.
{"title":"The FK5 Extension on the FK4 system","authors":"M. Lattanzi, L. Taff","doi":"10.1086/116613","DOIUrl":"https://doi.org/10.1086/116613","url":null,"abstract":"This paper reports on the computations necessary to place the FK5 Extension (epoch of place B1950.0) on the B1950.0/FK4 system from its published form and the availability of this version of the catalog. An application of the utility of the new version of the FK5 Extension, to the AGK3U, is given too. This confirms both the system of the AGK3U and the estimated values of its equatorial coordinate and proper motion mean errors. In addition, we have fully exploited the flexibility of the method of infinitely overlapping circles to compute a mean epoch of place/FK4 version of the FK5 Extension which we also make available. These modifications include taking into account the changes induced by the new system of general precession constants, adjusting for the e-terms of aberration, correcting for both the FK5/FK4 equinox offset and motion, and the FK5/FK4 positional and the proper motion systematic differences.","PeriodicalId":9423,"journal":{"name":"Bulletin of the American Astronomical Society","volume":"68 1","pages":"1231"},"PeriodicalIF":0.0,"publicationDate":"1993-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"77154406","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 1993-06-01DOI: 10.1016/0273-1177(93)90512-A
R. Lin, B. Dennis, R. Ramaty, A. Emslie, R. Canfield, G. Doschek
{"title":"Invited Talk: (The NASA High Energy Solar Physics (HESP) Mission for the Next Solar Maximum)","authors":"R. Lin, B. Dennis, R. Ramaty, A. Emslie, R. Canfield, G. Doschek","doi":"10.1016/0273-1177(93)90512-A","DOIUrl":"https://doi.org/10.1016/0273-1177(93)90512-A","url":null,"abstract":"","PeriodicalId":9423,"journal":{"name":"Bulletin of the American Astronomical Society","volume":"84 1","pages":"1180"},"PeriodicalIF":0.0,"publicationDate":"1993-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"78461008","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
A kinematic study has been carried out of the line-emitting gas in the Seyfert galaxy NGC 3516. The existence of two curved filaments in the central 2.5 kpc of this galaxy, which give Z-shaped appearance to its NLR. A precessing twin-jet model in which the line-emitting material is entrained by a precessing radio jet and kept ionized by the nuclear ionization field can explain the kinematic data of the brightest emission rather well. If this model is valid, this would make NGC 3516 the least luminous known active galaxy with a precessing jet. An alternative scenario assumes that the curved inner filaments represent gas entrained by a radio jet which is deflected by ram pressure from the rotation interstellar medium of the galaxy.
{"title":"On the origin of the Z-shaped narrow-line region in the Seyfert galaxy NGC 3516","authors":"S. Veilleux, R. Tully, J. Bland-Hawthorn","doi":"10.1086/116512","DOIUrl":"https://doi.org/10.1086/116512","url":null,"abstract":"A kinematic study has been carried out of the line-emitting gas in the Seyfert galaxy NGC 3516. The existence of two curved filaments in the central 2.5 kpc of this galaxy, which give Z-shaped appearance to its NLR. A precessing twin-jet model in which the line-emitting material is entrained by a precessing radio jet and kept ionized by the nuclear ionization field can explain the kinematic data of the brightest emission rather well. If this model is valid, this would make NGC 3516 the least luminous known active galaxy with a precessing jet. An alternative scenario assumes that the curved inner filaments represent gas entrained by a radio jet which is deflected by ram pressure from the rotation interstellar medium of the galaxy.","PeriodicalId":9423,"journal":{"name":"Bulletin of the American Astronomical Society","volume":"3 1","pages":"1428"},"PeriodicalIF":0.0,"publicationDate":"1993-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"79374976","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 1993-01-01DOI: 10.1007/978-94-011-1964-1_23
R. Thomas, W. Neupert, W. Thompson
{"title":"Calibrated Solar EUV Spectrum from Serts","authors":"R. Thomas, W. Neupert, W. Thompson","doi":"10.1007/978-94-011-1964-1_23","DOIUrl":"https://doi.org/10.1007/978-94-011-1964-1_23","url":null,"abstract":"","PeriodicalId":9423,"journal":{"name":"Bulletin of the American Astronomical Society","volume":"11 1","pages":"195-198"},"PeriodicalIF":0.0,"publicationDate":"1993-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"72965014","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
J. Graham, K. Matthews, J. Greenstein, G. Neugebauer, C. Tinney, S. E. Persson
We have obtained I, J, H, Kf and L' photometry and infrared spectroscopy (λ/Δλ ≃ 100) from 1.2-2.4 µm of the unusual emission line M star PC0025+0447. The near infrared photometry shows that this star has infrared colors which are comparable to the latest M dwarf stars such as LHS 2924 and LHS 2065. The infrared colors of PC0025+0447 establish that this star is a dwarf and not a distant giant. The infrared spectrum is dominated by strong H_2O absorption bands, and these bands are the strongest measured in any dwarf. Since H_2O band strength increases with decreasing temperature it is very likely that PC0025-f 0447 is substantially cooler than any of the stars calibrated by Berriman & Reid [MNRAS, 227, 315 (1987)], i.e. T_(eff) 10^9 yr) H burning star, with M ≃ 0.08 M_☉, or a younger brown dwarf.
{"title":"Infrared photometry and spectroscopy of the brown dwarf candidate PC0025+0447","authors":"J. Graham, K. Matthews, J. Greenstein, G. Neugebauer, C. Tinney, S. E. Persson","doi":"10.1086/116377","DOIUrl":"https://doi.org/10.1086/116377","url":null,"abstract":"We have obtained I, J, H, Kf and L' photometry and infrared spectroscopy (λ/Δλ ≃ 100) from 1.2-2.4 µm of the unusual emission line M star PC0025+0447. The near infrared photometry shows that this star has infrared colors which are comparable to the latest M dwarf stars such as LHS 2924 and LHS 2065. The infrared colors of PC0025+0447 establish that this star is a dwarf and not a distant giant. The infrared spectrum is dominated by strong H_2O absorption bands, and these bands are the \u0000strongest measured in any dwarf. Since H_2O band strength increases with decreasing temperature it is very likely that PC0025-f 0447 is substantially cooler than any of the stars calibrated by Berriman & Reid [MNRAS, 227, 315 (1987)], i.e. T_(eff) 10^9 yr) H burning star, with M ≃ 0.08 M_☉, or a younger brown dwarf.","PeriodicalId":9423,"journal":{"name":"Bulletin of the American Astronomical Society","volume":"2010 1","pages":"1416"},"PeriodicalIF":0.0,"publicationDate":"1992-11-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"86311271","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Deep photometric observations of stars in three fields of the LMC are presented, and these data are interpreted using synthetic CMDs and LFs generated from overshoot models. The field CMDs and LFs with a star formation rate that experienced a large increase (4 +/- 0.5) x 10 exp 9 yr ago is successfully modeled. The precise age of this 'burst' depends sensitively on the characteristics of the models. Classical (i.e., nonovershoot) models yield a burst age about 2 x 10 exp 9 yr younger than the value obtained. An initial mass function with slope of 2.35 (the Salpeter value) and a mean field star metallicity of Fe/H of about -0.7 are consistent with the photometric data and LFs. It is suggested that the star formation rate in the LMC was globally quite low during at least the first half of its lifetime, and that a major event triggered a substantial and relatively sudden increase in the star formation rate throughout the entire LMC which persisted for several 10 exp 9 yr and even up to the present epoch in some parts of that galaxy.
{"title":"The star formation history of the Large Magellanic Cloud","authors":"G. Bertelli, M. Mateo, C. Chiosi, A. Bressan","doi":"10.1086/171163","DOIUrl":"https://doi.org/10.1086/171163","url":null,"abstract":"Deep photometric observations of stars in three fields of the LMC are presented, and these data are interpreted using synthetic CMDs and LFs generated from overshoot models. The field CMDs and LFs with a star formation rate that experienced a large increase (4 +/- 0.5) x 10 exp 9 yr ago is successfully modeled. The precise age of this 'burst' depends sensitively on the characteristics of the models. Classical (i.e., nonovershoot) models yield a burst age about 2 x 10 exp 9 yr younger than the value obtained. An initial mass function with slope of 2.35 (the Salpeter value) and a mean field star metallicity of Fe/H of about -0.7 are consistent with the photometric data and LFs. It is suggested that the star formation rate in the LMC was globally quite low during at least the first half of its lifetime, and that a major event triggered a substantial and relatively sudden increase in the star formation rate throughout the entire LMC which persisted for several 10 exp 9 yr and even up to the present epoch in some parts of that galaxy.","PeriodicalId":9423,"journal":{"name":"Bulletin of the American Astronomical Society","volume":"2 1","pages":"949"},"PeriodicalIF":0.0,"publicationDate":"1992-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"85473875","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
The C III spectrum is studied quantitatively under both optically thin and optically thick conditions, yielding term populations and line/multiplet intensities for column lengths from zero to 10 exp 18/sq cm. The roles of escape probabilities and line profiles in the calculation are discussed in some detail. It is shown that use of the fully integrated escape factor, rather than the more appropriate monodirectional escape probability, can lead to appreciable errors in calculated intensities. The results for populations and intensities make it possible to identify two unassigned features in the solar EUV spectrum of Vernazza and Reeves (1978) as C III multiplets, and to establish that an unidentified infrared solar feature at 8500.32 A, seen in both absorption (Fraunhofer) and emission (chromospheric) spectra, is the C III transition 2s3s(1S)-2s3p(1P). Voigt parameters for the C III lines and multiplets, obtained by a modified semiclassical method are tabulated. A new, unambiguous notation for the numerous line ratios present in a typical spectrum, which is argued to be an improvement over present arbitrary notations, is proposed and used.
C III光谱在光学薄和光学厚的条件下进行定量研究，在柱长度从0到10 exp 18/sq cm的范围内，产生术语种群和线/多重强度。详细讨论了逃逸概率和线型在计算中的作用。结果表明，使用完全集成的逃逸因子，而不是更合适的单向逃逸概率，会导致计算强度的明显误差。种群和强度的结果使我们有可能在Vernazza和Reeves(1978)的太阳EUV光谱中识别两个未分配的特征为C III多重星，并确定在8500.32 A的未识别的太阳红外特征，在吸收(弗劳恩霍夫)和发射(色球)光谱中都可以看到，是C III跃迁23s (1S)-2s3p(1P)。本文列出了用改进的半经典方法得到的Cⅲ系和多联体的Voigt参数。提出并使用了一种新的，明确的符号，用于典型光谱中存在的众多线比，这被认为是对目前任意符号的改进。
{"title":"The Optically Thick C III Spectrum: I. Term Populations and Multiplet Intensities at Lower Optical Depths","authors":"A. Bhatia, S. O. Kastner","doi":"10.1086/191648","DOIUrl":"https://doi.org/10.1086/191648","url":null,"abstract":"The C III spectrum is studied quantitatively under both optically thin and optically thick conditions, yielding term populations and line/multiplet intensities for column lengths from zero to 10 exp 18/sq cm. The roles of escape probabilities and line profiles in the calculation are discussed in some detail. It is shown that use of the fully integrated escape factor, rather than the more appropriate monodirectional escape probability, can lead to appreciable errors in calculated intensities. The results for populations and intensities make it possible to identify two unassigned features in the solar EUV spectrum of Vernazza and Reeves (1978) as C III multiplets, and to establish that an unidentified infrared solar feature at 8500.32 A, seen in both absorption (Fraunhofer) and emission (chromospheric) spectra, is the C III transition 2s3s(1S)-2s3p(1P). Voigt parameters for the C III lines and multiplets, obtained by a modified semiclassical method are tabulated. A new, unambiguous notation for the numerous line ratios present in a typical spectrum, which is argued to be an improvement over present arbitrary notations, is proposed and used.","PeriodicalId":9423,"journal":{"name":"Bulletin of the American Astronomical Society","volume":"74 1","pages":"1203"},"PeriodicalIF":0.0,"publicationDate":"1992-03-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"83975222","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
{"title":"Massive star formation in galactic disks.","authors":"S. Ryder","doi":"10.25911/5D6E501F72B69","DOIUrl":"https://doi.org/10.25911/5D6E501F72B69","url":null,"abstract":"","PeriodicalId":9423,"journal":{"name":"Bulletin of the American Astronomical Society","volume":"37 1","pages":"1210"},"PeriodicalIF":0.0,"publicationDate":"1992-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"73812631","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 1992-01-01DOI: 10.1007/3-540-55256-1_309
D. Bohlender, C. T. Bolton, G. Walker
{"title":"Variable Hα emission in the helium-strong star δ orionis C","authors":"D. Bohlender, C. T. Bolton, G. Walker","doi":"10.1007/3-540-55256-1_309","DOIUrl":"https://doi.org/10.1007/3-540-55256-1_309","url":null,"abstract":"","PeriodicalId":9423,"journal":{"name":"Bulletin of the American Astronomical Society","volume":"9 1","pages":"221-223"},"PeriodicalIF":0.0,"publicationDate":"1992-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"82014566","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
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