Lines of O IV and S IV in the Goddard High-Resolution Spectrograph spectrum of RR Tel: constraints on atomic data
(1999) In Monthly Notices of the Royal Astronomical Society 303(3). p.41-46- Abstract
- High signal-to-noise ratio spectra of RR Tel obtained at medium resolution with the Goddard High-Resolution Spectrograph (GHRS) on the Hubble Space Telescope (HST) are used to test available atomic data for the O IV 2s(2)2p P-2-2s2p(2) P-4 multiplet (UV 0.01). The fine-structure intervals of the 2s2p(2) P-4 term given by Moore (1983) appear to need revision. The flux ratios of lines within multiplet UV (0.01), which have a common upper level, depend only on transition probabilities. The observed flux ratio of lines from the P-4(3/2) level differs from that predicted by theory, but this difference cannot be attributed to a blend with a line of S IV]. At the electron densities in the RR Tel nebula, other flux ratios give information on the... (More)
- High signal-to-noise ratio spectra of RR Tel obtained at medium resolution with the Goddard High-Resolution Spectrograph (GHRS) on the Hubble Space Telescope (HST) are used to test available atomic data for the O IV 2s(2)2p P-2-2s2p(2) P-4 multiplet (UV 0.01). The fine-structure intervals of the 2s2p(2) P-4 term given by Moore (1983) appear to need revision. The flux ratios of lines within multiplet UV (0.01), which have a common upper level, depend only on transition probabilities. The observed flux ratio of lines from the P-4(3/2) level differs from that predicted by theory, but this difference cannot be attributed to a blend with a line of S IV]. At the electron densities in the RR Tel nebula, other flux ratios give information on the relative electron excitation rates between the P-2 and P-4 fine-structure levels. Using the collision strengths calculated by Zhang, Graziani & Pradhan, the rate to the P-4(5/2) level, relative to the rates to the other J states, appears to be underestimated by similar to 10 per cent, which is within the expected uncertainty of 20 per cent. We also discuss the S IV 3s(2)3p P-2-3s3p(2) P-4 multiplet. (Less)
Please use this url to cite or link to this publication:
https://lup.lub.lu.se/record/3919497
- author
- Harper, GM ; Jordan, C ; Judge, PG ; Robinson, RD ; Carpenter, KG and Brage, Tomas LU
- organization
- publishing date
- 1999
- type
- Contribution to journal
- publication status
- published
- subject
- keywords
- RR Tel, individual, ultraviolet, stars, atomic data, symbiotic, binaries
- in
- Monthly Notices of the Royal Astronomical Society
- volume
- 303
- issue
- 3
- pages
- 41 - 46
- publisher
- Oxford University Press
- external identifiers
-
- wos:000079153600002
- scopus:0002477318
- ISSN
- 1365-2966
- DOI
- 10.1046/j.1365-8711.1999.02392.x
- language
- English
- LU publication?
- yes
- additional info
- The information about affiliations in this record was updated in December 2015. The record was previously connected to the following departments: Physics, science (011013100)
- id
- d933c93c-4dd8-4143-89ef-4213e2eab753 (old id 3919497)
- date added to LUP
- 2016-04-01 12:14:08
- date last changed
- 2022-01-27 00:49:39
@article{d933c93c-4dd8-4143-89ef-4213e2eab753,
abstract = {{High signal-to-noise ratio spectra of RR Tel obtained at medium resolution with the Goddard High-Resolution Spectrograph (GHRS) on the Hubble Space Telescope (HST) are used to test available atomic data for the O IV 2s(2)2p P-2-2s2p(2) P-4 multiplet (UV 0.01). The fine-structure intervals of the 2s2p(2) P-4 term given by Moore (1983) appear to need revision. The flux ratios of lines within multiplet UV (0.01), which have a common upper level, depend only on transition probabilities. The observed flux ratio of lines from the P-4(3/2) level differs from that predicted by theory, but this difference cannot be attributed to a blend with a line of S IV]. At the electron densities in the RR Tel nebula, other flux ratios give information on the relative electron excitation rates between the P-2 and P-4 fine-structure levels. Using the collision strengths calculated by Zhang, Graziani & Pradhan, the rate to the P-4(5/2) level, relative to the rates to the other J states, appears to be underestimated by similar to 10 per cent, which is within the expected uncertainty of 20 per cent. We also discuss the S IV 3s(2)3p P-2-3s3p(2) P-4 multiplet.}},
author = {{Harper, GM and Jordan, C and Judge, PG and Robinson, RD and Carpenter, KG and Brage, Tomas}},
issn = {{1365-2966}},
keywords = {{RR Tel; individual; ultraviolet; stars; atomic data; symbiotic; binaries}},
language = {{eng}},
number = {{3}},
pages = {{41--46}},
publisher = {{Oxford University Press}},
series = {{Monthly Notices of the Royal Astronomical Society}},
title = {{Lines of O IV and S IV in the Goddard High-Resolution Spectrograph spectrum of RR Tel: constraints on atomic data}},
url = {{http://dx.doi.org/10.1046/j.1365-8711.1999.02392.x}},
doi = {{10.1046/j.1365-8711.1999.02392.x}},
volume = {{303}},
year = {{1999}},
}