Line Evolution of the Nova V5587 Sgr from Early to Nebula Phase
The spectral evolution of the nova V5587 Sgr has been monitored at Koyama Astronomical Observatory and Higashi-Hiroshima Observatory, Japan, from the early to nebula phase. The nova rebrightened several times. The spectra during the early phase showed emission lines of H α, H β, O I, He I, He II, N...
| Main Authors: | , , , , , , |
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| Format: | Article |
| Language: | English |
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CTU Central Library
2015-02-01
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| Series: | Acta Polytechnica CTU Proceedings |
| Online Access: | https://ojs.cvut.cz/ojs/index.php/APP/article/view/2908 |
| _version_ | 1811327398877069312 |
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| author | T. Kajikawa A. Arai M. Nagashima H. Kawakita M. Yamanaka K. Kawabata S. Kiyota |
| author_facet | T. Kajikawa A. Arai M. Nagashima H. Kawakita M. Yamanaka K. Kawabata S. Kiyota |
| author_sort | T. Kajikawa |
| collection | DOAJ |
| description | The spectral evolution of the nova V5587 Sgr has been monitored at Koyama Astronomical Observatory and Higashi-Hiroshima Observatory, Japan, from the early to nebula phase. The nova rebrightened several times. The spectra during the early phase showed emission lines of H α, H β, O I, He I, He II, N II, Fe II. Nova V5587 Sgr is classified into the Fe II type. The helium abundance of the nova is estimated as <em>N</em>(He)/<em>N</em>(H) = 0.134 ± 0.09. The light curve, the spectral evolution, and the helium abundance in V5587 Sgr are similar to those of the nova PW Vul. |
| first_indexed | 2024-04-13T15:06:55Z |
| format | Article |
| id | doaj.art-e487e8f7ad3f4f3481b422f3ca0e98f7 |
| institution | Directory Open Access Journal |
| issn | 2336-5382 |
| language | English |
| last_indexed | 2024-04-13T15:06:55Z |
| publishDate | 2015-02-01 |
| publisher | CTU Central Library |
| record_format | Article |
| series | Acta Polytechnica CTU Proceedings |
| spelling | doaj.art-e487e8f7ad3f4f3481b422f3ca0e98f72022-12-22T02:42:08ZengCTU Central LibraryActa Polytechnica CTU Proceedings2336-53822015-02-012124224510.14311/APP.2015.02.02422670Line Evolution of the Nova V5587 Sgr from Early to Nebula PhaseT. Kajikawa0A. Arai1M. Nagashima2H. Kawakita3M. Yamanaka4K. Kawabata5S. KiyotaKyoto Sangyo University, Koyama Astronomical ObservatoryKyoto Sangyo University, Koyama Astronomical ObservatoryKyoto Sangyo University, Koyama Astronomical ObservatoryKyoto Sangyo University, Koyama Astronomical ObservatoryHiroshima University Kyoto University Konan UniversityHiroshima UniversityThe spectral evolution of the nova V5587 Sgr has been monitored at Koyama Astronomical Observatory and Higashi-Hiroshima Observatory, Japan, from the early to nebula phase. The nova rebrightened several times. The spectra during the early phase showed emission lines of H α, H β, O I, He I, He II, N II, Fe II. Nova V5587 Sgr is classified into the Fe II type. The helium abundance of the nova is estimated as <em>N</em>(He)/<em>N</em>(H) = 0.134 ± 0.09. The light curve, the spectral evolution, and the helium abundance in V5587 Sgr are similar to those of the nova PW Vul.https://ojs.cvut.cz/ojs/index.php/APP/article/view/2908 |
| spellingShingle | T. Kajikawa A. Arai M. Nagashima H. Kawakita M. Yamanaka K. Kawabata S. Kiyota Line Evolution of the Nova V5587 Sgr from Early to Nebula Phase Acta Polytechnica CTU Proceedings |
| title | Line Evolution of the Nova V5587 Sgr from Early to Nebula Phase |
| title_full | Line Evolution of the Nova V5587 Sgr from Early to Nebula Phase |
| title_fullStr | Line Evolution of the Nova V5587 Sgr from Early to Nebula Phase |
| title_full_unstemmed | Line Evolution of the Nova V5587 Sgr from Early to Nebula Phase |
| title_short | Line Evolution of the Nova V5587 Sgr from Early to Nebula Phase |
| title_sort | line evolution of the nova v5587 sgr from early to nebula phase |
| url | https://ojs.cvut.cz/ojs/index.php/APP/article/view/2908 |
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