Pub Date : 1981-12-31DOI: 10.1017/S1539299600003725
G. Herzberg
{"title":"The Interplay of Molecular Spectroscopy and Astronomy","authors":"G. Herzberg","doi":"10.1017/S1539299600003725","DOIUrl":"https://doi.org/10.1017/S1539299600003725","url":null,"abstract":"","PeriodicalId":422890,"journal":{"name":"Highlights of Astronomy","volume":"57 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"1981-12-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"133084991","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 : 1977-03-01DOI: 10.1007/978-94-010-1250-8_69
T. Snow, E. Jenkins
{"title":"A Catalogue of 0.2 Å Resolution Far-Ultraviolet Stellar Spectra Measured with Copernicus","authors":"T. Snow, E. Jenkins","doi":"10.1007/978-94-010-1250-8_69","DOIUrl":"https://doi.org/10.1007/978-94-010-1250-8_69","url":null,"abstract":"","PeriodicalId":422890,"journal":{"name":"Highlights of Astronomy","volume":"363 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"1977-03-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"122341223","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 : 1973-10-01DOI: 10.1007/978-94-010-2211-8_36
J. Einasto
{"title":"The Correlation Between Kinematical Properties and Ages of Stellar Populations","authors":"J. Einasto","doi":"10.1007/978-94-010-2211-8_36","DOIUrl":"https://doi.org/10.1007/978-94-010-2211-8_36","url":null,"abstract":"","PeriodicalId":422890,"journal":{"name":"Highlights of Astronomy","volume":"1 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"1973-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"116668515","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 : 1900-01-01DOI: 10.1017/S1539299600017585
C. Emerich, L. Jaffel, J. Clarke, G. Ballester
. The asymmetry observed in the H-Lya profiles measured near the Jovian equatorial limbs by the STIS/HST spectrograph is interpreted as due to H atoms propagating in the upper Jovian atmosphere with velocities ~ 80 km/s relative to Jupiter's rotation. A qualitative scenario is suggested to correlate these energetic H atoms to energetic neutral particles recently detected by Cassini at higher altitudes. Owing to the unique capabilities of the STIS/HST spectro-imager, Jovian H-Lya line profiles were obtained on different locations of Jupiter, with un precedented accuracy. For both observations sets obtained around the 2000 and 2001 oppositions, the Jovian line profiles reveal a distinct asymmetry near the two opposite equatorial limbs: the red wings are in excess relative to the blue ones for the receding limbs, the reverse holding for the approaching limbs. We attributed these additional Ly-a emissions to resonant scattering of the solar Ly-a emission by a high altitude population of fast neutral H located close to the approaching and receding limbs. The measured velocities, ranging between a few tens of km/s and ~ 170 km/s relative to Jupiter, reveal a population of neutral H in super corotation with Jupiter. Such a population of fast neutral atoms is likely to be produced by charge exchange between neutral H and ener getic atmospheric and magnetospheric charged particles which are accelerated by the intense Jovian magnetic field. As the large observed velocities evoke energetic neutral atoms (ENA) widely studied for the Earth's atmosphere, we suggest that multiple charge exchange processes should similarly produce sec
{"title":"Hot Hydrogen in the Jovian Corona","authors":"C. Emerich, L. Jaffel, J. Clarke, G. Ballester","doi":"10.1017/S1539299600017585","DOIUrl":"https://doi.org/10.1017/S1539299600017585","url":null,"abstract":". The asymmetry observed in the H-Lya profiles measured near the Jovian equatorial limbs by the STIS/HST spectrograph is interpreted as due to H atoms propagating in the upper Jovian atmosphere with velocities ~ 80 km/s relative to Jupiter's rotation. A qualitative scenario is suggested to correlate these energetic H atoms to energetic neutral particles recently detected by Cassini at higher altitudes. Owing to the unique capabilities of the STIS/HST spectro-imager, Jovian H-Lya line profiles were obtained on different locations of Jupiter, with un precedented accuracy. For both observations sets obtained around the 2000 and 2001 oppositions, the Jovian line profiles reveal a distinct asymmetry near the two opposite equatorial limbs: the red wings are in excess relative to the blue ones for the receding limbs, the reverse holding for the approaching limbs. We attributed these additional Ly-a emissions to resonant scattering of the solar Ly-a emission by a high altitude population of fast neutral H located close to the approaching and receding limbs. The measured velocities, ranging between a few tens of km/s and ~ 170 km/s relative to Jupiter, reveal a population of neutral H in super corotation with Jupiter. Such a population of fast neutral atoms is likely to be produced by charge exchange between neutral H and ener getic atmospheric and magnetospheric charged particles which are accelerated by the intense Jovian magnetic field. As the large observed velocities evoke energetic neutral atoms (ENA) widely studied for the Earth's atmosphere, we suggest that multiple charge exchange processes should similarly produce sec","PeriodicalId":422890,"journal":{"name":"Highlights of Astronomy","volume":"92 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"1900-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"115665341","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 : 1900-01-01DOI: 10.1007/978-94-010-2211-8_22
A. R. Hyland
{"title":"Medium resolution stellar spectra in the two-micron region","authors":"A. R. Hyland","doi":"10.1007/978-94-010-2211-8_22","DOIUrl":"https://doi.org/10.1007/978-94-010-2211-8_22","url":null,"abstract":"","PeriodicalId":422890,"journal":{"name":"Highlights of Astronomy","volume":"44 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"1900-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"123082263","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 : 1900-01-01DOI: 10.1017/S1539299600017226
A. Moorwood
. Plans for future high-resolution infrared spectrometers on large groundbased telescopes, their capabilities and science goals are briefly reviewed.
． 简要回顾了未来大型地基望远镜上高分辨率红外光谱仪的计划、性能和科学目标。
{"title":"Future Groundbased High-Resolution IR Spectrometers","authors":"A. Moorwood","doi":"10.1017/S1539299600017226","DOIUrl":"https://doi.org/10.1017/S1539299600017226","url":null,"abstract":". Plans for future high-resolution infrared spectrometers on large groundbased telescopes, their capabilities and science goals are briefly reviewed.","PeriodicalId":422890,"journal":{"name":"Highlights of Astronomy","volume":"74 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"1900-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"121789050","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 : 1900-01-01DOI: 10.1017/S1539299600018098
J. Pasachoff
I report on American textbooks for kindergarten through highschool grades. Middle school, up through approximate age 15, is the last time American students are required to take science, and I provide statistics on the narrowing of the funnel containing those taking physics. I describe some recent curriculum and standards projects, and I discuss the recent “less is more” trend. I conclude with comments on whether textbooks are necessary and useful and discuss possible content and style of an ideal textbook.
{"title":"Textbooks for K-12 Astronomy","authors":"J. Pasachoff","doi":"10.1017/S1539299600018098","DOIUrl":"https://doi.org/10.1017/S1539299600018098","url":null,"abstract":"I report on American textbooks for kindergarten through highschool grades. Middle school, up through approximate age 15, is the last time American students are required to take science, and I provide statistics on the narrowing of the funnel containing those taking physics. I describe some recent curriculum and standards projects, and I discuss the recent “less is more” trend. I conclude with comments on whether textbooks are necessary and useful and discuss possible content and style of an ideal textbook.","PeriodicalId":422890,"journal":{"name":"Highlights of Astronomy","volume":"256 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"1900-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"121819392","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 : 1900-01-01DOI: 10.1017/S1539299600016968
C. Russell
{"title":"Dawn Discovery Mission: Symbiosis with 1 AU Observations","authors":"C. Russell","doi":"10.1017/S1539299600016968","DOIUrl":"https://doi.org/10.1017/S1539299600016968","url":null,"abstract":"","PeriodicalId":422890,"journal":{"name":"Highlights of Astronomy","volume":"59 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"1900-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"121820240","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 : 1900-01-01DOI: 10.1017/S1539299600020062
D. Lambert
“It takes little talent to see clearly what lies under one’s nose, a good deal of it to know in which direction to point that organ.” W. H. Auden Listening to the sequence of fine talks that have made up this Joint Discussion, I have been impressed by the veritable flood of new observations that bear on the question of the abundance ratios in the oldest stars. The flood is marked by depth and diversity, as ‘noses’ are being pointed in highly profitable directions. As an example of depth, I would note the extensive investigations reviewed by Andy McWilliam of the chemical compositions of very metal-poor stars where [Fe/H] ≃ -3 marks the upper end of the range defining the class. To characterize diversity, I draw attention to the analyses of quasar absorption line systems so ably discssed by Limin Lu who showed that the abundance ratios for the gas in such high z systems resemble ratios found from Galactic metal-poor stars. Of course, to many at this Joint Discussion the wealth and diversity did not come as a surprise. Indeed, I suspect that many of us pursue the topic of the composition of the first generations of stars because of the wealth and diversity of observational constraints that may now spawn a unified interpretation. Hopefully, the marvellous talks given here will pull in a few new minds - young and old - to ponder nucleosynthesis in very young galaxies and in our Galaxy in particular.
{"title":"A Retrospective Introduction","authors":"D. Lambert","doi":"10.1017/S1539299600020062","DOIUrl":"https://doi.org/10.1017/S1539299600020062","url":null,"abstract":"“It takes little talent to see clearly what lies under one’s nose, a good deal of it to know in which direction to point that organ.” W. H. Auden Listening to the sequence of fine talks that have made up this Joint Discussion, I have been impressed by the veritable flood of new observations that bear on the question of the abundance ratios in the oldest stars. The flood is marked by depth and diversity, as ‘noses’ are being pointed in highly profitable directions. As an example of depth, I would note the extensive investigations reviewed by Andy McWilliam of the chemical compositions of very metal-poor stars where [Fe/H] ≃ -3 marks the upper end of the range defining the class. To characterize diversity, I draw attention to the analyses of quasar absorption line systems so ably discssed by Limin Lu who showed that the abundance ratios for the gas in such high z systems resemble ratios found from Galactic metal-poor stars. Of course, to many at this Joint Discussion the wealth and diversity did not come as a surprise. Indeed, I suspect that many of us pursue the topic of the composition of the first generations of stars because of the wealth and diversity of observational constraints that may now spawn a unified interpretation. Hopefully, the marvellous talks given here will pull in a few new minds - young and old - to ponder nucleosynthesis in very young galaxies and in our Galaxy in particular.","PeriodicalId":422890,"journal":{"name":"Highlights of Astronomy","volume":"174 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"1900-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"124269368","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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