1998
DOI: 10.1086/306097
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Contribution of Type Ia and Type II Supernovae to Intracluster Medium Enrichment

Abstract: The origin of the chemical composition of the intracluster medium (ICM) is discussed in this paper. In particular, the contribution from Type Ia supernovae (SNe Ia) to the ICM enrichment is shown to exist by adopting the fitting formulas which have been used in the analysis of the solar system abundances.Our analysis means that we can use the frequency of SNe Ia relative to SNe II as the better measure than M Fe,SNIa /M Fe,total for estimating the contribution of SNe Ia. Moreover, the chemical compositions of … Show more

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Cited by 26 publications
(29 citation statements)
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“…Scaling our measured abundance ratios to the meteoric abundance scale of Anders & Grevesse (1989), we determine [Mg/Fe] ∼0.00, [Si/Fe] ∼0.02 and [S/Fe] ∼0.16. Comparing these values with the supernova yield models of Nagataki & Sato (1998), our observed [Si/Fe] ratio implies a mass fraction of the iron enrichment resulting from type Ia supernova, M Fe,SNIa M Fe,total , in the range 0.55–0.9 (where the limits cover the full range of models examined by these authors). For spherical type II supernovae, a mass fraction in the range M Fe,SNIa M Fe,total ∼0.7–0.85 is preferred.…”
Section: The Element Abundances In Ngc 4636mentioning
confidence: 61%
“…Scaling our measured abundance ratios to the meteoric abundance scale of Anders & Grevesse (1989), we determine [Mg/Fe] ∼0.00, [Si/Fe] ∼0.02 and [S/Fe] ∼0.16. Comparing these values with the supernova yield models of Nagataki & Sato (1998), our observed [Si/Fe] ratio implies a mass fraction of the iron enrichment resulting from type Ia supernova, M Fe,SNIa M Fe,total , in the range 0.55–0.9 (where the limits cover the full range of models examined by these authors). For spherical type II supernovae, a mass fraction in the range M Fe,SNIa M Fe,total ∼0.7–0.85 is preferred.…”
Section: The Element Abundances In Ngc 4636mentioning
confidence: 61%
“…However, the lower sulphur yields associated with aspherical Type II explosion models imply somewhat lower values, depending on the degree of asphericity and the precise SNIa enrichment model used. In particular, the observed [S/Fe] ratio appears inconsistent with enrichment models incorporating both a high degree of asphericity in the SNeII explosions and simple deflagration of the Type Ia supernovae (Nagataki & Sato 1998). Comparing the observed [S/Fe] value with Gibson et al (1997) indicates In contrast to previous results (Mushotzky et al 1996; Gibson et al 1997), our observations do not indicate a severe deficiency of sulphur with respect to the other α ‐elements, when compared with the theoretical predictions (at least for models incorporating relatively low degree of asphericity in the Type II supernovae).…”
Section: The Abundances Of Elements In the Virgo And Centaurus Clusmentioning
confidence: 90%
“…Recently, a number of studies (Gibson, Lowenstein & Mushotzky 1997;Ishimaru & Arimoto 1997;Nagataki & Sato 1998;Dupke & White 2000a) have presented detailed predictions for the aelement abundances in the ICM, as a function of the fraction of the iron enrichment due to Type Ia supernovae, using a variety of theoretical supernovae models. Scaling the observed abundance ratios for the central regions of the Centaurus and Virgo clusters to the meteoric abundance scale of Anders & Grevesse (1989), as used in the theoretical calculations, we determine mean, unweighted abundance ratios of MgaFe , 20X63Y SiaFe , 0X00 and SaFe , 0X02X Thus the [Si/Fe] and [S/Fe] ratios in the central regions of the Centaurus and Virgo clusters are in good agreement with the solar meteoric values.…”
Section: Comparison With Supernovae Enrichment Modelsmentioning
confidence: 99%
“…In x 4.3 we show that the abundance ratio of Si to Fe is close to the solar ratio. Note that among -elements, the abundance measurement of Si is least uncertain because of its strong, isolated emission features; the theoretical yields of Si are also the best determined, with the least amount of scatter between model predictions (e.g., Gibson et al 1997;Nagataki & Sato 1998). With SN yields taken from Gibson et al (1997) and converted to the revised solar values given by Grevesse & Sauval (1998), the measured abundance ratio of Si to Fe (near solar) indicates that 60%-80% of the detected iron mass is produced in Type Ia SNe.…”
Section: Elemental Abundances and Supernovv A Yieldsmentioning
confidence: 99%