Near‐Infrared and Ultraviolet Spectrophotometry of Symbiotic Novae

Rudy, R. J.; Meier, Steven R.; Rossano, G. S.; Lynch, D. K.; Puetter, R. C.; Erwin, Peter

doi:10.1086/313197

“…4, so this may be consistent. The same feature is also seen in the symbiotic nova PU Vul by Rudy et al (1999) and again identified as Fe II λλ 9176-9205.…”

Section: The λ 9220å Featuresupporting

confidence: 62%

Late Spectral Evolution of the Ejecta and Reverse Shock in Sn 1987a

Fransson

¹

,

Larsson

²

,

Spyromilio³

et al. 2013

ApJ

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We present observations with VLT and HST of the broad emission lines from the inner ejecta and reverse shock of SN 1987A from 1999 Feb. until 2012 Jan. (days 4381 -9100 after explosion). We detect broad lines from Hα, Hβ, Mg I], Na I, [O I], [Ca II] and a feature at ∼ 9220Å. We identify the latter line with Mg II λλ 9218, 9244, which is most likely pumped by Lyα fluorescence. Hα, and Hβ both have a centrally peaked component, extending to ∼ 4500 km s −1 and a very broad component extending to 11, 000 km s −1 , while the other lines have only the central component. The low velocity component comes from unshocked ejecta, heated mainly by X-rays from the circumstellar environment, whereas the broad component comes from faster ejecta passing through the reverse shock, created by the collision with the circumstellar ring. The flux in Hα from the reverse shock has increased by a factor of 4 − 6 from 2000 to 2007. After that there is a tendency of flattening of the light curve, similar to what may be seen in soft X-rays and in the optical lines from the shocked ring. The core component seen in Hα, [Ca II] and Mg II has experienced a similar increase, which is consistent with that found from HST photometry. The ring-like morphology of the ejecta is explained as a result of the X-ray illumination, depositing energy outside of the core of the ejecta. The energy deposition of the external X-rays is calculated using explosion models for SN 1987A and we predict that the outer parts of the unshocked ejecta will continue to brighten because of this. We finally discuss evidence for dust in the ejecta from line asymmetries.

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“…In these systems, despite the much smaller outburst amplitudes compared to those observed in novae, the total energy associated with the outburst may significantly exceed that of a classical nova. Currently very little is known about the line-emitting regions associated with the outburst of a symbiotic nova because of the long timescales to reach the maximum and the very much slower decays (Rudy et al, 1999). Symbiotics also fall in the category of the supersoft X-ray sources (Greiner, 1996) making them potential SN Ia progenitors (Hachisu et al, 1999).…”

Section: Symbiotic Starsmentioning

confidence: 99%

Ultraviolet Studies Of Interacting Binaries

Gäansicke

¹

,

Martino

²

,

Marsh

³

et al. 2006

Astrophys Space Sci

2

0

1

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Interacting Binaries consist of a variety of stellar objects in different stages of evolution and those containing accreting compact objects still represent a major challenge to our understanding of not only close binary evolution but also of the chemical evolution of the Galaxy. These end-points of binary star evolution are ideal laboratories for the study of accretion and outflow processes, and provide insight on matter under extreme physical conditions. One of the key-questions of fundamental relevance is the nature of SN Ia progenitors. The study of accreting compact binary systems relies on observations over the entire electromagnetic spectrum and we outline here those unresolved questions for which access to the ultraviolet range is vital, as they cannot be addressed by observations in any other spectral region. B.T. Gäansicke ( ) · T.R. Marsh

show abstract

“…In these systems, despite the much smaller outburst amplitudes compared to those observed in novae, the total energy associated with the outburst may significantly exceed that of a classical nova. Currently very little is known about the line-emitting regions associated with the outburst of a symbiotic nova because of the long timescales to reach the maximum and the very much slower decays (Rudy et al, 1999). Symbiotics also fall in the category of the supersoft X-ray sources (Greiner, 1996) making them potential SN Ia progenitors (Hachisu et al, 1999).…”

Section: Symbiotic Starsmentioning

confidence: 99%

Ultraviolet Studies of Interacting Binaries

Gänsicke

¹

,

Martino

²

,

Marsh

³

et al. 2006

Astrophys Space Sci

View full text Add to dashboard Cite

Interacting Binaries consist of a variety of stellar objects in different stages of evolution and those containing accreting compact objects still represent a major challenge to our understanding of not only close binary evolution but also of the chemical evolution of the Galaxy. These end-points of binary star evolution are ideal laboratories for the study of accretion and outflow processes, and provide insight on matter under extreme physical conditions. One of the key-questions of fundamental relevance is the nature of SN Ia progenitors. The study of accreting compact binary systems relies on observations over the entire electromagnetic spectrum and we outline here those unresolved questions for which access to the ultraviolet range is vital, as they cannot be addressed by observations in any other spectral region.

show abstract

Near‐Infrared and Ultraviolet Spectrophotometry of Symbiotic Novae

Cited by 18 publications

References 41 publications

Late Spectral Evolution of the Ejecta and Reverse Shock in Sn 1987a

Late Spectral Evolution of the Ejecta and Reverse Shock in Sn 1987a

Ultraviolet Studies Of Interacting Binaries

Ultraviolet Studies of Interacting Binaries

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