Fractional yields inferred from halo and thick disk stars

Linear [Q/H]-[O/H] relations, Q = Na, Mg, Si, Ca, Ti, Cr, Fe, Ni, are inferred from a sample (N = 67) of recently studied FGK-type dwarf stars in the solar neighbourhood including different populations (Nissen and Schuster 2010, Ramirez et al. 2012), namely LH (N = 24, low-α halo), HH (N = 25, high-α halo), KD (N = 16, thick disk), and OL (N = 2, globular cluster outliers). Regression line slope and intercept estimators and related variance estimators are determined. With regard to the straight line, [Q/H]=aQ[O/H]+bQ, sample stars are displayed along a "main sequence", [Q,O] = [aQ, bQ, ΔbQ], leaving aside the two OL stars, which, in most cases (e.g. Na), lie outside. The unit slope, aQ = 1, implies Q is a primary element synthesised via SNII progenitors in the presence of a universal stellar initial mass function (defined as simple primary element). In this respect, Mg, Si, Ti, show âQ = 1 within -+2^σâQ; Cr, Fe, Ni, within -+3^σâQ; Na, Ca, within -+r^σâQ, r < 3. The empirical, differential element abundance distributions are inferred from LH, HH, KD, HA = HH + KD subsamples, where related regression lines represent their theoretical counterparts within the framework of simple MCBR (multistage closed box + reservoir) chemical evolution models. Hence, the fractional yields, ^pQ/^pO, are determined and (as an example) a comparison is shown with their theoretical counterparts inferred from SNII progenitor nucleosynthesis under the assumption of a power-law stellar initial mass function. The generalized fractional yields, CQ=ZQ/ZaQ O, are determined regardless of the chemical evolution model. The ratio of outflow to star formation rate is compared for different populations in the framework of simple MCBR models. The opposite situation of element abundance variation entirely due to cosmic scatter is also considered under reasonable assumptions. The related differential element abundance distribution fits to the data, as well as its counterpart inferred in the opposite limit of instantaneous mixing in the presence of chemical evolution, while the latter is preferred for HA subsample. Ausführliche Beschreibung

Gespeichert in:

Autor*in:	Caimmi R. [verfasserIn]

Format:	E-Artikel
Sprache:	Englisch

Erschienen:	2013

Schlagwörter:	Galaxy: galaxy: evolution galaxy: formation stars: evolution stars: formation

Übergeordnetes Werk:	In: Serbian Astronomical Journal - Astronomical Observatory, Department of Astronomy, Belgrade, 2008, (2013), 187, Seite 19-41
Übergeordnetes Werk:	year:2013 ; number:187 ; pages:19-41

Links:	Link aufrufen Link aufrufen Link aufrufen Journal toc Journal toc

DOI / URN:	10.2298/SAJ130924004C

Katalog-ID:	DOAJ024016144

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spelling	10.2298/SAJ130924004C doi (DE-627)DOAJ024016144 (DE-599)DOAJee5f610867fd408387da316b8487b382 DE-627 ger DE-627 rakwb eng QB1-991 Caimmi R. verfasserin aut Fractional yields inferred from halo and thick disk stars 2013 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Linear [Q/H]-[O/H] relations, Q = Na, Mg, Si, Ca, Ti, Cr, Fe, Ni, are inferred from a sample (N = 67) of recently studied FGK-type dwarf stars in the solar neighbourhood including different populations (Nissen and Schuster 2010, Ramirez et al. 2012), namely LH (N = 24, low-α halo), HH (N = 25, high-α halo), KD (N = 16, thick disk), and OL (N = 2, globular cluster outliers). Regression line slope and intercept estimators and related variance estimators are determined. With regard to the straight line, [Q/H]=aQ[O/H]+bQ, sample stars are displayed along a "main sequence", [Q,O] = [aQ, bQ, ΔbQ], leaving aside the two OL stars, which, in most cases (e.g. Na), lie outside. The unit slope, aQ = 1, implies Q is a primary element synthesised via SNII progenitors in the presence of a universal stellar initial mass function (defined as simple primary element). In this respect, Mg, Si, Ti, show âQ = 1 within -+2^σâQ; Cr, Fe, Ni, within -+3^σâQ; Na, Ca, within -+r^σâQ, r < 3. The empirical, differential element abundance distributions are inferred from LH, HH, KD, HA = HH + KD subsamples, where related regression lines represent their theoretical counterparts within the framework of simple MCBR (multistage closed box + reservoir) chemical evolution models. Hence, the fractional yields, ^pQ/^pO, are determined and (as an example) a comparison is shown with their theoretical counterparts inferred from SNII progenitor nucleosynthesis under the assumption of a power-law stellar initial mass function. The generalized fractional yields, CQ=ZQ/ZaQ O, are determined regardless of the chemical evolution model. The ratio of outflow to star formation rate is compared for different populations in the framework of simple MCBR models. The opposite situation of element abundance variation entirely due to cosmic scatter is also considered under reasonable assumptions. The related differential element abundance distribution fits to the data, as well as its counterpart inferred in the opposite limit of instantaneous mixing in the presence of chemical evolution, while the latter is preferred for HA subsample. Galaxy: galaxy: evolution galaxy: formation stars: evolution stars: formation Astronomy In Serbian Astronomical Journal Astronomical Observatory, Department of Astronomy, Belgrade, 2008 (2013), 187, Seite 19-41 (DE-627)538218460 (DE-600)2378699-1 18209289 nnns year:2013 number:187 pages:19-41 https://doi.org/10.2298/SAJ130924004C kostenfrei https://doaj.org/article/ee5f610867fd408387da316b8487b382 kostenfrei http://www.doiserbia.nb.rs/img/doi/1450-698X/2013/1450-698X1300004C.pdf kostenfrei https://doaj.org/toc/1450-698X Journal toc kostenfrei https://doaj.org/toc/1820-9289 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_206 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2003 GBV_ILN_2005 GBV_ILN_2009 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2055 GBV_ILN_2111 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 2013 187 19-41
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allfieldsSound	10.2298/SAJ130924004C doi (DE-627)DOAJ024016144 (DE-599)DOAJee5f610867fd408387da316b8487b382 DE-627 ger DE-627 rakwb eng QB1-991 Caimmi R. verfasserin aut Fractional yields inferred from halo and thick disk stars 2013 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Linear [Q/H]-[O/H] relations, Q = Na, Mg, Si, Ca, Ti, Cr, Fe, Ni, are inferred from a sample (N = 67) of recently studied FGK-type dwarf stars in the solar neighbourhood including different populations (Nissen and Schuster 2010, Ramirez et al. 2012), namely LH (N = 24, low-α halo), HH (N = 25, high-α halo), KD (N = 16, thick disk), and OL (N = 2, globular cluster outliers). Regression line slope and intercept estimators and related variance estimators are determined. With regard to the straight line, [Q/H]=aQ[O/H]+bQ, sample stars are displayed along a "main sequence", [Q,O] = [aQ, bQ, ΔbQ], leaving aside the two OL stars, which, in most cases (e.g. Na), lie outside. The unit slope, aQ = 1, implies Q is a primary element synthesised via SNII progenitors in the presence of a universal stellar initial mass function (defined as simple primary element). In this respect, Mg, Si, Ti, show âQ = 1 within -+2^σâQ; Cr, Fe, Ni, within -+3^σâQ; Na, Ca, within -+r^σâQ, r < 3. The empirical, differential element abundance distributions are inferred from LH, HH, KD, HA = HH + KD subsamples, where related regression lines represent their theoretical counterparts within the framework of simple MCBR (multistage closed box + reservoir) chemical evolution models. Hence, the fractional yields, ^pQ/^pO, are determined and (as an example) a comparison is shown with their theoretical counterparts inferred from SNII progenitor nucleosynthesis under the assumption of a power-law stellar initial mass function. The generalized fractional yields, CQ=ZQ/ZaQ O, are determined regardless of the chemical evolution model. The ratio of outflow to star formation rate is compared for different populations in the framework of simple MCBR models. The opposite situation of element abundance variation entirely due to cosmic scatter is also considered under reasonable assumptions. The related differential element abundance distribution fits to the data, as well as its counterpart inferred in the opposite limit of instantaneous mixing in the presence of chemical evolution, while the latter is preferred for HA subsample. Galaxy: galaxy: evolution galaxy: formation stars: evolution stars: formation Astronomy In Serbian Astronomical Journal Astronomical Observatory, Department of Astronomy, Belgrade, 2008 (2013), 187, Seite 19-41 (DE-627)538218460 (DE-600)2378699-1 18209289 nnns year:2013 number:187 pages:19-41 https://doi.org/10.2298/SAJ130924004C kostenfrei https://doaj.org/article/ee5f610867fd408387da316b8487b382 kostenfrei http://www.doiserbia.nb.rs/img/doi/1450-698X/2013/1450-698X1300004C.pdf kostenfrei https://doaj.org/toc/1450-698X Journal toc kostenfrei https://doaj.org/toc/1820-9289 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_206 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2003 GBV_ILN_2005 GBV_ILN_2009 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2055 GBV_ILN_2111 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 2013 187 19-41
language	English
source	In Serbian Astronomical Journal (2013), 187, Seite 19-41 year:2013 number:187 pages:19-41
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author	Caimmi R.
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issn	18209289
topic_title	QB1-991 Fractional yields inferred from halo and thick disk stars Galaxy: galaxy: evolution galaxy: formation stars: evolution stars: formation
topic	misc QB1-991 misc Galaxy: galaxy: evolution misc galaxy: formation misc stars: evolution misc stars: formation misc Astronomy
topic_unstemmed	misc QB1-991 misc Galaxy: galaxy: evolution misc galaxy: formation misc stars: evolution misc stars: formation misc Astronomy
topic_browse	misc QB1-991 misc Galaxy: galaxy: evolution misc galaxy: formation misc stars: evolution misc stars: formation misc Astronomy
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title	Fractional yields inferred from halo and thick disk stars
ctrlnum	(DE-627)DOAJ024016144 (DE-599)DOAJee5f610867fd408387da316b8487b382
title_full	Fractional yields inferred from halo and thick disk stars
author_sort	Caimmi R.
journal	Serbian Astronomical Journal
journalStr	Serbian Astronomical Journal
callnumber-first-code	Q
lang_code	eng
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author_browse	Caimmi R.
class	QB1-991
format_se	Elektronische Aufsätze
author-letter	Caimmi R.
doi_str_mv	10.2298/SAJ130924004C
title_sort	fractional yields inferred from halo and thick disk stars
callnumber	QB1-991
title_auth	Fractional yields inferred from halo and thick disk stars
abstract	Linear [Q/H]-[O/H] relations, Q = Na, Mg, Si, Ca, Ti, Cr, Fe, Ni, are inferred from a sample (N = 67) of recently studied FGK-type dwarf stars in the solar neighbourhood including different populations (Nissen and Schuster 2010, Ramirez et al. 2012), namely LH (N = 24, low-α halo), HH (N = 25, high-α halo), KD (N = 16, thick disk), and OL (N = 2, globular cluster outliers). Regression line slope and intercept estimators and related variance estimators are determined. With regard to the straight line, [Q/H]=aQ[O/H]+bQ, sample stars are displayed along a "main sequence", [Q,O] = [aQ, bQ, ΔbQ], leaving aside the two OL stars, which, in most cases (e.g. Na), lie outside. The unit slope, aQ = 1, implies Q is a primary element synthesised via SNII progenitors in the presence of a universal stellar initial mass function (defined as simple primary element). In this respect, Mg, Si, Ti, show âQ = 1 within -+2^σâQ; Cr, Fe, Ni, within -+3^σâQ; Na, Ca, within -+r^σâQ, r < 3. The empirical, differential element abundance distributions are inferred from LH, HH, KD, HA = HH + KD subsamples, where related regression lines represent their theoretical counterparts within the framework of simple MCBR (multistage closed box + reservoir) chemical evolution models. Hence, the fractional yields, ^pQ/^pO, are determined and (as an example) a comparison is shown with their theoretical counterparts inferred from SNII progenitor nucleosynthesis under the assumption of a power-law stellar initial mass function. The generalized fractional yields, CQ=ZQ/ZaQ O, are determined regardless of the chemical evolution model. The ratio of outflow to star formation rate is compared for different populations in the framework of simple MCBR models. The opposite situation of element abundance variation entirely due to cosmic scatter is also considered under reasonable assumptions. The related differential element abundance distribution fits to the data, as well as its counterpart inferred in the opposite limit of instantaneous mixing in the presence of chemical evolution, while the latter is preferred for HA subsample.
abstractGer	Linear [Q/H]-[O/H] relations, Q = Na, Mg, Si, Ca, Ti, Cr, Fe, Ni, are inferred from a sample (N = 67) of recently studied FGK-type dwarf stars in the solar neighbourhood including different populations (Nissen and Schuster 2010, Ramirez et al. 2012), namely LH (N = 24, low-α halo), HH (N = 25, high-α halo), KD (N = 16, thick disk), and OL (N = 2, globular cluster outliers). Regression line slope and intercept estimators and related variance estimators are determined. With regard to the straight line, [Q/H]=aQ[O/H]+bQ, sample stars are displayed along a "main sequence", [Q,O] = [aQ, bQ, ΔbQ], leaving aside the two OL stars, which, in most cases (e.g. Na), lie outside. The unit slope, aQ = 1, implies Q is a primary element synthesised via SNII progenitors in the presence of a universal stellar initial mass function (defined as simple primary element). In this respect, Mg, Si, Ti, show âQ = 1 within -+2^σâQ; Cr, Fe, Ni, within -+3^σâQ; Na, Ca, within -+r^σâQ, r < 3. The empirical, differential element abundance distributions are inferred from LH, HH, KD, HA = HH + KD subsamples, where related regression lines represent their theoretical counterparts within the framework of simple MCBR (multistage closed box + reservoir) chemical evolution models. Hence, the fractional yields, ^pQ/^pO, are determined and (as an example) a comparison is shown with their theoretical counterparts inferred from SNII progenitor nucleosynthesis under the assumption of a power-law stellar initial mass function. The generalized fractional yields, CQ=ZQ/ZaQ O, are determined regardless of the chemical evolution model. The ratio of outflow to star formation rate is compared for different populations in the framework of simple MCBR models. The opposite situation of element abundance variation entirely due to cosmic scatter is also considered under reasonable assumptions. The related differential element abundance distribution fits to the data, as well as its counterpart inferred in the opposite limit of instantaneous mixing in the presence of chemical evolution, while the latter is preferred for HA subsample.
abstract_unstemmed	Linear [Q/H]-[O/H] relations, Q = Na, Mg, Si, Ca, Ti, Cr, Fe, Ni, are inferred from a sample (N = 67) of recently studied FGK-type dwarf stars in the solar neighbourhood including different populations (Nissen and Schuster 2010, Ramirez et al. 2012), namely LH (N = 24, low-α halo), HH (N = 25, high-α halo), KD (N = 16, thick disk), and OL (N = 2, globular cluster outliers). Regression line slope and intercept estimators and related variance estimators are determined. With regard to the straight line, [Q/H]=aQ[O/H]+bQ, sample stars are displayed along a "main sequence", [Q,O] = [aQ, bQ, ΔbQ], leaving aside the two OL stars, which, in most cases (e.g. Na), lie outside. The unit slope, aQ = 1, implies Q is a primary element synthesised via SNII progenitors in the presence of a universal stellar initial mass function (defined as simple primary element). In this respect, Mg, Si, Ti, show âQ = 1 within -+2^σâQ; Cr, Fe, Ni, within -+3^σâQ; Na, Ca, within -+r^σâQ, r < 3. The empirical, differential element abundance distributions are inferred from LH, HH, KD, HA = HH + KD subsamples, where related regression lines represent their theoretical counterparts within the framework of simple MCBR (multistage closed box + reservoir) chemical evolution models. Hence, the fractional yields, ^pQ/^pO, are determined and (as an example) a comparison is shown with their theoretical counterparts inferred from SNII progenitor nucleosynthesis under the assumption of a power-law stellar initial mass function. The generalized fractional yields, CQ=ZQ/ZaQ O, are determined regardless of the chemical evolution model. The ratio of outflow to star formation rate is compared for different populations in the framework of simple MCBR models. The opposite situation of element abundance variation entirely due to cosmic scatter is also considered under reasonable assumptions. The related differential element abundance distribution fits to the data, as well as its counterpart inferred in the opposite limit of instantaneous mixing in the presence of chemical evolution, while the latter is preferred for HA subsample.
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container_issue	187
title_short	Fractional yields inferred from halo and thick disk stars
url	https://doi.org/10.2298/SAJ130924004C https://doaj.org/article/ee5f610867fd408387da316b8487b382 http://www.doiserbia.nb.rs/img/doi/1450-698X/2013/1450-698X1300004C.pdf https://doaj.org/toc/1450-698X https://doaj.org/toc/1820-9289
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up_date	2024-07-03T20:45:05.936Z
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