Matches in SemOpenAlex for { <https://semopenalex.org/work/W2885087496> ?p ?o ?g. }
- W2885087496 endingPage "61" @default.
- W2885087496 startingPage "61" @default.
- W2885087496 abstract "There is now strong evidence that the close binary fraction (P < 10$^4$ days; a < 10 AU) of solar-type stars ($M_1$ = 0.6-1.5M$_{odot}$) decreases significantly with metallicity. Although early surveys showed that the observed spectroscopic binary (SB) fractions in the galactic disk and halo are similar (e.g., Carney-Latham sample), these studies did not correct for incompleteness. In this study, we examine five different surveys and thoroughly account for their underlying selection biases to measure the intrinsic occurrence rate of close solar-type binaries. We re-analyze: (1) a volume-limited sample of solar-type stars, (2) an SB survey of high-proper-motion stars, (3) various SB samples of metal-poor giants, (4) the APOGEE survey of radial velocity (RV) variables, and (5) Kepler eclipsing binaries (EBs). The observed APOGEE RV variability fraction and Kepler EB fraction both decrease by a factor of $approx$4 across $-$1.0 < [Fe/H] < 0.5 at the 22$sigma$ and 9$sigma$ confidence levels, respectively. After correcting for incompleteness, all five samples exhibit a quantitatively consistent anti-correlation between the intrinsic close binary fraction (a < 10 AU) and metallicity: $F_{rm close}$ = 53%$pm$12%, 40%$pm$6%, 24%$pm$4%, and 10%$pm$3% at [Fe/H] = $-$3.0, $-$1.0, $-$0.2 (mean field metallicity), and +0.5, respectively. We present fragmentation models that explain why the close binary fraction of solar-type stars strongly decreases with metallicity while the wide binary fraction, close binary fraction of OB stars, and initial mass function are all constant across $-$1.5 < [Fe/H] < 0.5. The majority of solar-type stars with [Fe/H] < $-$1.0 will interact with a stellar companion, which has profound implications for binary evolution in old and metal-poor environments such as the galactic halo, bulge, thick disk, globular clusters, dwarf galaxies, and high-redshift universe." @default.
- W2885087496 created "2018-08-22" @default.
- W2885087496 creator A5041111005 @default.
- W2885087496 creator A5066165480 @default.
- W2885087496 creator A5085910426 @default.
- W2885087496 date "2019-04-16" @default.
- W2885087496 modified "2023-10-12" @default.
- W2885087496 title "The Close Binary Fraction of Solar-type Stars Is Strongly Anticorrelated with Metallicity" @default.
- W2885087496 cites W1559350678 @default.
- W2885087496 cites W1562571124 @default.
- W2885087496 cites W1582881973 @default.
- W2885087496 cites W1639285581 @default.
- W2885087496 cites W1974140367 @default.
- W2885087496 cites W1976178453 @default.
- W2885087496 cites W1977033153 @default.
- W2885087496 cites W1984303403 @default.
- W2885087496 cites W1989436099 @default.
- W2885087496 cites W1990564060 @default.
- W2885087496 cites W1991823040 @default.
- W2885087496 cites W1994356380 @default.
- W2885087496 cites W1994570599 @default.
- W2885087496 cites W1996984257 @default.
- W2885087496 cites W1999197191 @default.
- W2885087496 cites W2001478608 @default.
- W2885087496 cites W2003332061 @default.
- W2885087496 cites W2005048610 @default.
- W2885087496 cites W2006615500 @default.
- W2885087496 cites W2007958786 @default.
- W2885087496 cites W2009821926 @default.
- W2885087496 cites W2011569645 @default.
- W2885087496 cites W2014983184 @default.
- W2885087496 cites W2017576190 @default.
- W2885087496 cites W2021062241 @default.
- W2885087496 cites W2024680894 @default.
- W2885087496 cites W2028041709 @default.
- W2885087496 cites W2029061901 @default.
- W2885087496 cites W2029077494 @default.
- W2885087496 cites W2029343094 @default.
- W2885087496 cites W2029733876 @default.
- W2885087496 cites W2035322651 @default.
- W2885087496 cites W2036179433 @default.
- W2885087496 cites W2036303070 @default.
- W2885087496 cites W2038094450 @default.
- W2885087496 cites W2038836191 @default.
- W2885087496 cites W2041251533 @default.
- W2885087496 cites W2047022889 @default.
- W2885087496 cites W2048389787 @default.
- W2885087496 cites W2048570620 @default.
- W2885087496 cites W2051431923 @default.
- W2885087496 cites W2052502986 @default.
- W2885087496 cites W2052528558 @default.
- W2885087496 cites W2052603028 @default.
- W2885087496 cites W2055534454 @default.
- W2885087496 cites W2055745258 @default.
- W2885087496 cites W2058926260 @default.
- W2885087496 cites W2059365121 @default.
- W2885087496 cites W2059879627 @default.
- W2885087496 cites W2061759127 @default.
- W2885087496 cites W2068882637 @default.
- W2885087496 cites W2070606946 @default.
- W2885087496 cites W2071733898 @default.
- W2885087496 cites W2072956639 @default.
- W2885087496 cites W2075787667 @default.
- W2885087496 cites W2079349148 @default.
- W2885087496 cites W2081038018 @default.
- W2885087496 cites W2082971238 @default.
- W2885087496 cites W2083521327 @default.
- W2885087496 cites W2085143106 @default.
- W2885087496 cites W2088308551 @default.
- W2885087496 cites W2091152621 @default.
- W2885087496 cites W2094756736 @default.
- W2885087496 cites W2097068720 @default.
- W2885087496 cites W2101001011 @default.
- W2885087496 cites W2101983354 @default.
- W2885087496 cites W2105878215 @default.
- W2885087496 cites W2126700402 @default.
- W2885087496 cites W2127823605 @default.
- W2885087496 cites W2129495060 @default.
- W2885087496 cites W2132579896 @default.
- W2885087496 cites W2133970979 @default.
- W2885087496 cites W2137885638 @default.
- W2885087496 cites W2138693252 @default.
- W2885087496 cites W2142428021 @default.
- W2885087496 cites W2148392241 @default.
- W2885087496 cites W2148547933 @default.
- W2885087496 cites W2149196484 @default.
- W2885087496 cites W2150034833 @default.
- W2885087496 cites W2152030864 @default.
- W2885087496 cites W2152115442 @default.
- W2885087496 cites W2157791991 @default.
- W2885087496 cites W2162462253 @default.
- W2885087496 cites W2163745499 @default.
- W2885087496 cites W2165265566 @default.
- W2885087496 cites W2167013981 @default.
- W2885087496 cites W2176148042 @default.
- W2885087496 cites W2203831943 @default.
- W2885087496 cites W2204423677 @default.
- W2885087496 cites W2205127315 @default.