QUANTIFYING THE CARBON ABUNDANCES IN THE SECONDARY STARS OF SS CYGNI, RU PEGASI, AND GK PERSEI

Journal Article · Sun Nov 15 00:00:00 EST 2015 · Astronomical Journal (Online)

DOI:https://doi.org/10.1088/0004-6256/150/5/142· OSTI ID:22520113

Harrison, Thomas E. ^[1]

---

1. Department of Astronomy, New Mexico State University, Box 30001, MSC 4500, Las Cruces, NM 88003-8001 (United States)

We use a modified version of MOOG to generate large grids of synthetic spectra in an attempt to derive quantitative abundances for three CVs (GK Per, RU Peg, and SS Cyg) by comparing the models to moderate resolution (R ∼ 25,000) K-band spectra obtained with NIRSPEC on Keck. For each of the three systems we find solar, or slightly sub-solar values for [Fe/H], but significant deficits of carbon: for SS Cyg we find [C/Fe] = −0.50, for RU Peg [C/Fe] = −0.75, and for GK Per [C/Fe] = −1.00. We show that it is possible to use lower resolution (R ∼ 2000) spectra to quantify carbon deficits. We examine realistic veiling scenarios and find that emission from H i or CO cannot reproduce the observations.

• OSTI ID: 22520113
• Journal Information: Astronomical Journal (Online), Vol. 150, Issue 5; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 1538-3881
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
CARBON
CARBON MONOXIDE
COMPARATIVE EVALUATIONS
ELEMENT ABUNDANCE
EMISSION SPECTRA
EMISSION SPECTROSCOPY
HYDROGEN
IRON
NOVAE
RESOLUTION
STAR MODELS