Abundance anomalies in CP Crucis (Nova Crux 1996)

James E. Lyke; X. P. Koenig; M. J. Barlow; R. D. Gehrz; Charles E. Woodward; Sumner Starrfield; D. Péquignot; A. Evans; A. Salama; R. González-Riestra; Matthew A. Greenhouse; R. M. Hjellming; Terry J. Jones; Joachim Krautter; H. B. Öoglman; R. Mark Wagner; S. L. Lumsden; R. E. Williams

doi:10.1086/376477

Abundance anomalies in CP Crucis (Nova Crux 1996)

James E. Lyke, X. P. Koenig, M. J. Barlow, R. D. Gehrz, Charles E. Woodward, Sumner Starrfield, D. Péquignot, A. Evans, A. Salama, R. González-Riestra, Matthew A. Greenhouse, R. M. Hjellming, Terry J. Jones, Joachim Krautter, H. B. Öoglman, R. Mark Wagner, S. L. Lumsden, R. E. Williams

Physics

Research output: Contribution to journal › Article › peer-review

16 Scopus citations

Abstract

We present spectroscopic observations of the classical nova CP Crucis (Nova Crux 1996) obtained with the Infrared Space Observatory Short Wavelength Spectrometer (ISO SWS) and the Anglo-Australian Telescope using both the Infrared Imaging Spectrograph and the Royal Greenwich Observatory Spectrograph. From the expansion parallax, we find that CP Crucis lies at a distance of 2.6 ± 0.5 kpc and reached a maximum My of - 8.7 at 0.96 days after discovery. We find abundance enhancements versus solar by mass of 75, 17, and 27 for N, O, and Ne, respectively. Additionally, we constrain the Mg abundance in the ejecta to be approximately solar. Abundance analysis suggests CP Crucis is an old Population I binary system. Combining the strong N and Ne abundances with the relatively low Mg abundance and a Ne/O ratio of 0.5, we propose that CP Crucis is an example of the "missing link" between CO and ONeMg novae.

Original language	English (US)
Pages (from-to)	993-1005
Number of pages	13
Journal	Astronomical Journal
Volume	126
Issue number	2 1772
DOIs	https://doi.org/10.1086/376477
State	Published - Aug 2003

Keywords

Circumstellar matter
Novae, cataclysmic variables
Stars: individual (Nova Crux 1996, CP Crucis)

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.1086/376477

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Lyke, J. E., Koenig, X. P., Barlow, M. J., Gehrz, R. D., Woodward, C. E., Starrfield, S., Péquignot, D., Evans, A., Salama, A., González-Riestra, R., Greenhouse, M. A., Hjellming, R. M., Jones, T. J., Krautter, J., Öoglman, H. B., Mark Wagner, R., Lumsden, S. L., & Williams, R. E. (2003). Abundance anomalies in CP Crucis (Nova Crux 1996). Astronomical Journal, 126(2 1772), 993-1005. https://doi.org/10.1086/376477

Lyke, JE, Koenig, XP, Barlow, MJ, Gehrz, RD, Woodward, CE, Starrfield, S, Péquignot, D, Evans, A, Salama, A, González-Riestra, R, Greenhouse, MA, Hjellming, RM, Jones, TJ, Krautter, J, Öoglman, HB, Mark Wagner, R, Lumsden, SL & Williams, RE 2003, 'Abundance anomalies in CP Crucis (Nova Crux 1996)', Astronomical Journal, vol. 126, no. 2 1772, pp. 993-1005. https://doi.org/10.1086/376477

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title = "Abundance anomalies in CP Crucis (Nova Crux 1996)",

abstract = "We present spectroscopic observations of the classical nova CP Crucis (Nova Crux 1996) obtained with the Infrared Space Observatory Short Wavelength Spectrometer (ISO SWS) and the Anglo-Australian Telescope using both the Infrared Imaging Spectrograph and the Royal Greenwich Observatory Spectrograph. From the expansion parallax, we find that CP Crucis lies at a distance of 2.6 ± 0.5 kpc and reached a maximum My of - 8.7 at 0.96 days after discovery. We find abundance enhancements versus solar by mass of 75, 17, and 27 for N, O, and Ne, respectively. Additionally, we constrain the Mg abundance in the ejecta to be approximately solar. Abundance analysis suggests CP Crucis is an old Population I binary system. Combining the strong N and Ne abundances with the relatively low Mg abundance and a Ne/O ratio of 0.5, we propose that CP Crucis is an example of the {"}missing link{"} between CO and ONeMg novae.",

keywords = "Circumstellar matter, Novae, cataclysmic variables, Stars: individual (Nova Crux 1996, CP Crucis)",

author = "Lyke, {James E.} and Koenig, {X. P.} and Barlow, {M. J.} and Gehrz, {R. D.} and Woodward, {Charles E.} and Sumner Starrfield and D. P{\'e}quignot and A. Evans and A. Salama and R. Gonz{\'a}lez-Riestra and Greenhouse, {Matthew A.} and Hjellming, {R. M.} and Jones, {Terry J.} and Joachim Krautter and {\"O}oglman, {H. B.} and {Mark Wagner}, R. and Lumsden, {S. L.} and Williams, {R. E.}",

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T1 - Abundance anomalies in CP Crucis (Nova Crux 1996)

AU - Lyke, James E.

AU - Koenig, X. P.

AU - Barlow, M. J.

AU - Gehrz, R. D.

AU - Woodward, Charles E.

AU - Starrfield, Sumner

AU - Péquignot, D.

AU - Evans, A.

AU - Salama, A.

AU - González-Riestra, R.

AU - Greenhouse, Matthew A.

AU - Hjellming, R. M.

AU - Jones, Terry J.

AU - Krautter, Joachim

AU - Öoglman, H. B.

AU - Mark Wagner, R.

AU - Lumsden, S. L.

AU - Williams, R. E.

PY - 2003/8

Y1 - 2003/8

N2 - We present spectroscopic observations of the classical nova CP Crucis (Nova Crux 1996) obtained with the Infrared Space Observatory Short Wavelength Spectrometer (ISO SWS) and the Anglo-Australian Telescope using both the Infrared Imaging Spectrograph and the Royal Greenwich Observatory Spectrograph. From the expansion parallax, we find that CP Crucis lies at a distance of 2.6 ± 0.5 kpc and reached a maximum My of - 8.7 at 0.96 days after discovery. We find abundance enhancements versus solar by mass of 75, 17, and 27 for N, O, and Ne, respectively. Additionally, we constrain the Mg abundance in the ejecta to be approximately solar. Abundance analysis suggests CP Crucis is an old Population I binary system. Combining the strong N and Ne abundances with the relatively low Mg abundance and a Ne/O ratio of 0.5, we propose that CP Crucis is an example of the "missing link" between CO and ONeMg novae.

AB - We present spectroscopic observations of the classical nova CP Crucis (Nova Crux 1996) obtained with the Infrared Space Observatory Short Wavelength Spectrometer (ISO SWS) and the Anglo-Australian Telescope using both the Infrared Imaging Spectrograph and the Royal Greenwich Observatory Spectrograph. From the expansion parallax, we find that CP Crucis lies at a distance of 2.6 ± 0.5 kpc and reached a maximum My of - 8.7 at 0.96 days after discovery. We find abundance enhancements versus solar by mass of 75, 17, and 27 for N, O, and Ne, respectively. Additionally, we constrain the Mg abundance in the ejecta to be approximately solar. Abundance analysis suggests CP Crucis is an old Population I binary system. Combining the strong N and Ne abundances with the relatively low Mg abundance and a Ne/O ratio of 0.5, we propose that CP Crucis is an example of the "missing link" between CO and ONeMg novae.

KW - Circumstellar matter

KW - Novae, cataclysmic variables

KW - Stars: individual (Nova Crux 1996, CP Crucis)

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JF - Astronomical Journal

SN - 0004-6256

IS - 2 1772

ER -

Abundance anomalies in CP Crucis (Nova Crux 1996)

Abstract

Keywords

ASJC Scopus subject areas

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