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  • Super and massive AGB stars - II. Nucleosynthesis and yields - Z = 0.02, 0.008 and 0.004

     Doherty, Carolyn L.; Gil Pons, Pilar; Lau, Herbert B.; Lattanzio, John C.; Siess, Lionel
    Monthly notices of the Royal Astronomical Society
    Vol. 437, p. 195-214
    DOI: 10.1093/mnras/stt1877
    Date of publication: 2014-01
    Journal article

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    We have computed detailed evolution and nucleosynthesis models for super and massive asymptotic giant branch (AGB) stars over the mass range 6.5¿9.0¿M¿ in divisions of 0.5¿M¿ with metallicities Z = 0.02, 0.008 and 0.004. These calculations, in which we find third dredge-up and hot bottom burning, fill the gap between existing low- and intermediate-mass AGB star models and high-mass star models that become supernovae. For the considered metallicities, the composition of the yields is largely dominated by the thermodynamic conditions at the base of the convective envelope rather than by the pollution arising from third dredge-up. We investigate the effects of various uncertainties, related to the mass-loss rate, mixing length parameter, and the treatment of evolution after the envelope instability that develops near the end of the (super)AGB phase. Varying these parameters alters the yields mainly because of their impact on the amount of third dredge-up enrichment, and to a lesser extent on the hot bottom burning conditions. Our models produce significant amounts of 4He, 7Li (depending on the mass-loss formulation) 13C, 14N, 17O, 23Na, 25Mg, as well the radioactive isotope 26Al in agreement with previous investigation. In addition, our results show enrichment of 22Ne, 26Mg and 60Fe, as well as a substantial increase in our proxy neutron capture species representing all species heavier than iron. These stars may provide important contributions to the Galaxy's inventory of the heavier Mg isotopes, 14N, 7Li and 27Al.

  • On the necessity of composition-dependent low-temperature opacity in models of metal-poor Asymptotic Giant Branch stars

     Constantino, Thomas; Campbell, Simon W; Gil Pons, Pilar; Lattanzio, John C.
    Astrophysical journal
    DOI: 10.1088/0004-637X/784/1/56
    Date of publication: 2014
    Journal article

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    The vital importance of composition-dependent low-temperature opacity in low-mass (M <= 3 M ¿) asymptotic giant branch (AGB) stellar models of metallicity Z >= 0.001 has recently been demonstrated. Its significance to more metal-poor, intermediate-mass (M >= 2.5 M ¿) models has yet to be investigated. We show that its inclusion in lower-metallicity models ([Fe/H] <=-2) is essential and that there exists no threshold metallicity below which composition-dependent molecular opacity may be neglected. We find it to be crucial in all intermediate-mass models investigated ([Fe/H] <=-2 and 2.5 <= M/M ¿ <= 5), because of the evolution of the surface chemistry, including the orders of magnitude increase in the abundance of molecule-forming species. Its effect on these models mirrors that previously reported for higher-metallicity models¿increase in radius, decrease in T eff, faster mass loss, shorter thermally pulsing AGB lifetime, reduced enrichment in third dredge-up products (by a factor of 3-10), and an increase in the mass limit for hot bottom burning. We show that the evolution of low-metallicity models with composition-dependent low-temperature opacity is relatively independent of initial metal abundance because its contribution to the opacity is far outweighed by changes resulting from dredge-up. Our results imply a significant reduction in the expected number of nitrogen-enhanced metal-poor stars, which may help explain their observed paucity. We note that these findings are partially a product of the macrophysics adopted in our models, in particular, the Vassiliadis & Wood mass loss rate which is strongly dependent on radius.

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    Evolution and CNO yields of Z = 10-5 stars and possible effects on carbon-enhanced metal-poor production  Open access

     Gil Pons, Pilar; Doherty, Carolyn L.; Lau, Herbert B.; Campbell, Simon W; Suda, Takuma; Guilani, Shervin Mansouri; Gutierrez Cabello, Jorge Luis; Lattanzio, John C.
    Astronomy and astrophysics
    Vol. 557, p. 106-118Evolution and CNO yields of Z = 10-5 stars and possible effects on carbon-enhanced metal-poor production
    DOI: 10.1051/0004-6361/201321127
    Date of publication: 2013-09
    Journal article

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    Aims. Our main goals are to get a deeper insight into the evolution and final fates of intermediate-mass, extremely metal-poor (EMP) stars. We also aim to investigate the C, N, and O yields of these stars. Methods. Using the Monash University Stellar Evolution code MONSTAR we computed and analysed the evolution of stars of metallicity Z = 10-5 and masses between 4 and 9 M¿, from their main sequence until the late thermally pulsing (super) asymptotic giant branch, TP-(S)AGB phase. Results. Our model stars experience a strong C, N, and O envelope enrichment either due to the second dredge-up process, the dredge-out phenomenon, or the third dredge-up early during the TP-(S)AGB phase. Their late evolution is therefore similar to that of higher metallicity objects. When using a standard prescription for the mass loss rates during the TP-(S)AGB phase, the computed stars are able to lose most of their envelopes before their cores reach the Chandrasekhar mass (mCh), so our standard models do not predict the occurrence of SNI1/2 for Z = 10-5 stars. However, we find that the reduction of only one order of magnitude in the mass-loss rates, which are particularly uncertain at this metallicity, would prevent the complete ejection of the envelope, allowing the stars to either explode as an SNI1/2 or become an electron-capture SN. Our calculations stop due to an instability near the base of the convective envelope that hampers further convergence and leaves remnant envelope masses between 0.25 M¿ for our 4 M¿ model and 1.5 M¿ for our 9 M¿ model. We present two sets of C, N, and O yields derived from our full calculations and computed under two different assumptions, namely, that the instability causes a practically instant loss of the remnant envelope or that the stars recover and proceed with further thermal pulses. Conclusions. Our results have implications for the early chemical evolution of the Universe and might provide another piece for the puzzle of the carbon-enhanced EMP star problem.

    Aims. Our main goals are to get a deeper insight into the evolution and final fates of intermediate-mass, extremely metal-poor (EMP) stars. We also aim to investigate the C, N, and O yields of these stars. Methods. Using the Monash University Stellar Evolution code MONSTAR we computed and analysed the evolution of stars of metallicity Z = 10-5 and masses between 4 and 9 M¿, from their main sequence until the late thermally pulsing (super) asymptotic giant branch, TP-(S)AGB phase. Results. Our model stars experience a strong C, N, and O envelope enrichment either due to the second dredge-up process, the dredge-out phenomenon, or the third dredge-up early during the TP-(S)AGB phase. Their late evolution is therefore similar to that of higher metallicity objects. When using a standard prescription for the mass loss rates during the TP-(S)AGB phase, the computed stars are able to lose most of their envelopes before their cores reach the Chandrasekhar mass (mCh), so our standard models do not predict the occurrence of SNI1/2 for Z = 10-5 stars. However, we find that the reduction of only one order of magnitude in the mass-loss rates, which are particularly uncertain at this metallicity, would prevent the complete ejection of the envelope, allowing the stars to either explode as an SNI1/2 or become an electron-capture SN. Our calculations stop due to an instability near the base of the convective envelope that hampers further convergence and leaves remnant envelope masses between 0.25 M¿ for our 4 M¿ model and 1.5 M¿ for our 9 M¿ model. We present two sets of C, N, and O yields derived from our full calculations and computed under two different assumptions, namely, that the instability causes a practically instant loss of the remnant envelope or that the stars recover and proceed with further thermal pulses. Conclusions. Our results have implications for the early chemical evolution of the Universe and might provide another piece for the puzzle of the carbon-enhanced EMP star problem.

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    Transition of the stellar initial mass function explored using binary population synthesis  Open access

     Suda, Takuma; Komiya, Yutaka; Yamada, Shimako; Katsuta, Yutaka; Aoki, Wako; Gil Pons, Pilar; Doherty, Carolyn L.; Campbell, Simon W; Wood, Peter R.; Fujimoto, Masayuki Y.
    Monthly notices of the Royal Astronomical Society
    Vol. 432, p. 46-50
    DOI: 10.1093/mnrasl/slt033
    Date of publication: 2013
    Journal article

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    The stellar initial mass function (IMF) plays a crucial role in determining the number of surviving stars in galaxies, the chemical composition of the interstellar medium, and the distribution of light in galaxies. A key unsolved question is whether the IMF is universal in time and space. Here we use state-of-the-art results of stellar evolution to show that the IMF of our Galaxy made a transition from an IMF dominated by massive stars to the present-day IMF at an early phase of the Galaxy formation. Updated results from stellar evolution in a wide range of metallicities have been implemented in a binary population synthesis code, and compared with the observations of carbon-enhanced metal-poor (CEMP) stars in our Galaxy. We find that applying the present-day IMF to Galactic halo stars causes serious contradictions with four observable quantities connected with the evolution of AGB stars. Furthermore, a comparison between our calculations and the observations of CEMP stars may help us to constrain the transition metallicity for the IMF which we tentatively set at [Fe/H] = -2. A novelty of the current study is the inclusion of mass loss suppression in intermediate-mass AGB stars at low-metallicity. This significantly reduces the overproduction of nitrogen-enhanced stars that was a major problem in using the high-mass star dominated IMF in previous studies. Our results also demonstrate that the use of the present day IMF for all time in chemical evolution models results in the overproduction of Type I.5 supernovae. More data on stellar abundances will help to understand how the IMF has changed and what caused such a transition.

    The stellar initial mass function (IMF) plays a crucial role in determining the number of surviving stars in galaxies, the chemical composition of the interstellar medium, and the distribution of light in galaxies. A key unsolved question is whether the IMF is universal in time and space. Here we use state-of-the-art results of stellar evolution to show that the IMF of our Galaxy made a transition from an IMF dominated by massive stars to the present-day IMF at an early phase of the Galaxy formation. Updated results from stellar evolution in a wide range of metallicities have been implemented in a binary population synthesis code, and compared with the observations of carbon-enhanced metal-poor (CEMP) stars in our Galaxy. We find that applying the present-day IMF to Galactic halo stars causes serious contradictions with four observable quantities connected with the evolution of AGB stars. Furthermore, a comparison between our calculations and the observations of CEMP stars may help us to constrain the transition metallicity for the IMF which we tentatively set at [Fe/H] = -2. A novelty of the current study is the inclusion of mass loss suppression in intermediate-mass AGB stars at low-metallicity. This significantly reduces the overproduction of nitrogen-enhanced stars that was a major problem in using the high-mass star dominated IMF in previous studies. Our results also demonstrate that the use of the present day IMF for all time in chemical evolution models results in the overproduction of Type I.5 supernovae. More data on stellar abundances will help to understand how the IMF has changed and what caused such a transition.

  • Large-Scale Structure and the First Stars with the BOSS Quasar Absorption Spectra

     Gil Pons, Pilar; Miralda Escudé, Jordi
    Competitive project

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  • The end of super AGB and massive AGB stars - I. The instabilities that determine the final mass of AGB stars

     Lau, Herbert B.; Gil Pons, Pilar; Doherty, Carolyn L.; Lattanzio, John C.
    Astronomy and astrophysics
    Vol. 542, p. 1-10
    DOI: 10.1051/0004-6361/201218826
    Date of publication: 2012-06
    Journal article

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    Production of short-lived radioactive nuclei in super asymptotic giant branch star  Open access

     Doherty, Carolyn L.; Lugaro, M.; Lau, Herbert B.; Siess, Lionel; Lattanzio, John C.; Gil Pons, Pilar
    Meteoritic and Planetary Sciences
    Vol. 47, p. 5159
    DOI: 10.1111/j.1945-5100.2012.01401_2.x
    Date of publication: 2012-08-08
    Journal article

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  • Bridging the mass divide: super & massive AGB star yields

     Doherty, Carolyn L.; Gil Pons, Pilar; Lau, Herbert B.; Lattanzio, John C.
    Date of publication: 2012
    Book chapter

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    Production of short-lived radioactive nuclei in Super Asymptotic Giant Branch stars  Open access

     Doherty, Carolyn L.; Lugaro, M.; Lau, Herbert B.; Siess, Lionel; Lattanzio, John C.; Gil Pons, Pilar
    Annual Meeting of the Meteoritical Society
    Presentation's date: 2012
    Presentation of work at congresses

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  • The evolution and C, N and O yields of intermediate-mass Z = 10-5 stars in isolation and in close binary systems  Open access

     Gil Pons, Pilar; Doherty, Carolyn L.; Suda, Takuma; Campbell, Simon W; Lau, Herbert B.; Mansouri Guilani, Shervin; Lattanzio, John C.
    First Stars
    p. 358-360
    DOI: 10.1063/1.4754386
    Presentation's date: 2012
    Presentation of work at congresses

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    We have computed the evolution of Z = 10−5 stars of masses between 4 and 9 M , from their main sequence till the late TP-(S)AGB phase.We use a recent version of the Mount Stromlo Stellar Evolution code, in which molecular opacities include the effects of variable C/O abundances ratio, [1]. By computing hundreds (or thousands) of thermal pulses, we have been able either to remove the bulk of the stellar envelopes or to obtain stellar cores very close to MCh. Using [2] prescription for the mass loss rates the computed stars lose their envelopes before their cores reach MCh. This would forbid the occurrence of SN 1.5 for Z = 10−5 stars. Nevertheless the results by [3] suggest that the former prescription might overestimate the mass-loss rates. Therefore we have decreased the rates by [2]. For all the cases we present, even a decrease of one order of magnitude let the stellar cores reach MCh before the envelope is lost. Therefore the occurrence of SN1.5 at Z = 10 −5 and their potential contribution to the chemical evolution of the Universe should not be discarded. We consider the combined effects of the deep/corrosive 2 nd dredge-up and Roche Lobe Overflow (RLOF) during the E-AGB to help to constrain the contribution of massive Z = 10 −5 AGB stars to the CEMPs problem. Our results have implications for the chemical evolution of the Universe and might provide another piece for the puzzle of the CEMPs problem.

  • Transition of the initial mass function in the galaxy based on binary population synthesis

     Suda, Takuma; Komiya, Yutaka; Yamada, Shimako; Katsuta, Yutaka; Aoki, Wako; Gil Pons, Pilar; Doherty, Carolyn L.; Campbell, Simon W; Wood, Peter R.; Fujimoto, Masayuki Y.
    First Stars
    p. 421-423
    DOI: 10.1063/1.4754407
    Presentation's date: 2012
    Presentation of work at congresses

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  • S-process Nucleosynthesis in SAGB Stars

     Lau, Herbert B.; Doherty, Carolyn L.; Gil Pons, Pilar; Lattanzio, John C.
    Date of publication: 2011-12-01
    Book chapter

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  • Super asymptotic giant branch stars. I - Evolution code comparison

     Doherty, Carolyn L.; Siess, Lionel; Lattanzio, John C.; Gil Pons, Pilar
    Monthly notices of the Royal Astronomical Society
    Vol. 401, p. 1453-1464
    Date of publication: 2010-01-01
    Journal article

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    We present an extensive set of detailed stellar models in the mass range 7.7–10.5M over the metallicity range Z = 10−5–0.02. These models were produced using the Monash University version of the Mount Stromlo Stellar Structure Program (MONSTAR) and follow the evolution from the pre-main sequence to the first thermal pulse of these super asymptotic giant branch stars. A quantitative comparison is made to the study of Siess. Prior to this study, only qualitative comparisons and code validations existed in this critical mass range, and the large variations in the literature were largely unexplained. The comparison presented here is particularly detailed due to the standardization of the input physics, where possible. The minimum initial mass of star which ignites carbon, Mup, was found to agree within 0.2M between the codes over the entire metallicity range.We find exceptional agreement in the model results between these two codes for all stages of evolution up to and including carbon burning. For additional comparison, we also present results from the EVOLVE code, a modified version of the IBEN code as described in Gil-Pons, Guti´errez & Garc´ıa-Berro for some important variables during the carbon burning phase. Several numerical tests showed that the carbon burning phase is weakly dependent on the spatial resolution but that inadequate temporal resolution alters the behaviour of the convective zones.We also discovered that stars just below Mup may experience a carbon flash that is not followed by the development of the flame. Such aborted carbon burning models thus preserve a CO core surrounding by a 0.2–0.3M shell of partially burnt carbon material. We present a simplified algorithm for calculating carbon burning that only relies on tracking two species, 12C and 16O, but which tests show works quite accurately for the a wide range of initial masses and compositions

  • The upper mass limit for the formation of TP-SAGB stars and the dredge-out phenomenon

     Gil Pons, Pilar; Doherty, Carolyn L.
    Memorie della Societá Astronomica Italiana
    Vol. 81, num. 4, p. 974-979
    Date of publication: 2010-12-01
    Journal article

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  • The upper-mass limit for the formation of super-agb stars and the dredge-out phenomenon

     Gil Pons, Pilar; Doherty, Carolyn L.
    Memorie della Societá Astronomica Italiana
    Vol. 81, p. 574-579
    Date of publication: 2010
    Journal article

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    We have computed the evolution of Super-AGB stars from the main sequence and up to a few hundred thermal pulses, with special attention to the low metallicity cases (Z = 10 10; 10 5; 10 4 and 10 3). Our computations have been performed using time– dependent mixing and new opacity tables that admit variations in the abundances of carbon and oxygen. By following the evolution along the main central burning stages and the early TP-SAGB, we resolve the upper mass limits for the formation of TP-SAGB stars and determine the mass range at which the dredge-out phenomenon occurs. This phenomenon involves the merger of a convective shell sustained by helium burning at the top of the degenerate core with the hydrogen–rich convective envelope and the occurrence of a hydrogen flash. The dredge–out allows elements synthesised through helium burning to be transported to the stellar surfaces and therefore it can a ect the initial composition of the TP-SAGB stars.

  • S-process Nucleosynthesis in SAGB Stars

     Lau, Herbert B.; Doherty, Carolyn L.; Gil Pons, Pilar; Lattanzio, John C.
    Why Galaxies Care about AGB Stars II: Shining Examples and Common Inhabitants.
    p. 45-51
    Presentation's date: 2010-08-16
    Presentation of work at congresses

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  • The upper mass limit for the formation of TP-SAGB stars and the dredge-out phenomenon

     Gil Pons, Pilar
    Torino Workshop on Asymptotic Giant Branch Nucleosynthesis
    p. 974-979
    Presentation's date: 2010-01-21
    Presentation of work at congresses

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  • On the Fate of Extremely Low Metallicity Stars

     Gil Pons, Pilar; Gutierrez Cabello, Jorge Luis; Garcia-berro Montilla, Enrique; Althaus, Leandro G.
    AIP Conference proceedings
    Vol. 1001, p. 71-78
    DOI: 10.1063/1.2916992
    Date of publication: 2008-12-01
    Journal article

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    On the fate of extremely low metallicity stars  Open access

     Gil Pons, Pilar; Gutierrez Cabello, Jorge Luis; Garcia-berro Montilla, Enrique; Althaus, Leandro G.
    AIP Conference proceedings
    Vol. 1001, p. 71-78
    DOI: 10.1063/1.2916992
    Date of publication: 2008
    Journal article

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    We have computed and analyzed the evolution of intermediate-mass stars of metallicity Z = 10−5 from the main sequence until the early stages of the TP-(S)AGB phase. In order to check the influence of mixing we have performed our calculations using two different evolutionary codes, EVOLVE — which does not include diffusion but allows for overshooting— and LPCODE, which includes diffusion and overshooting “à-la-Herwig”. Important differences appear during the TP– AGB phase, as the calculations done with EVOLVE lead to an almost negligible third dredge-up, whereas the sequences computed with LPCODE show important third dredge-up and, therefore, significant enrichment in metals of the envelope. This fact has consequences on the strength of the winds during the TP-AGB phase and, ultimately, on the final fate of the considered stars. Also, the models computed with LPCODE show strong double flashes produced by the ingestion of protons on the helium burning shell.

    Postprint (author’s final draft)

  • Astronomy and astrophysics

     Gil Pons, Pilar
    Collaboration in journals

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  • SAGB stars: the missing link? (ARC Discovery PROYECTOs, DP0807317)

     Lattanzio, John C.; Gil Pons, Pilar
    Competitive project

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    Is there a chance for primordial SNeI1/2?  Open access

     Gil Pons, Pilar; Gutierrez Cabello, Jorge Luis; Garcia-berro Montilla, Enrique
    Proceedings of Science
    Vol. 13, p. 1-14
    Date of publication: 2007-09
    Journal article

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    The evolution of primordial stars of initial masses between 5 and 10 M⊙ has been computed and analyzed in order to determine the nature of the remnants of massive intermediate–mass primordial stars and to check the influence of overshooting in their evolution. We have obtained the values for the limiting masses of Population III progenitor stars leading to carbon–oxygen and oxygen–neon compact cores. We have also obtained the limiting mass for which isolated primordial stars would lead to core–collapse supernovae after the end of the main central burning phases. Considering a moderate amount of overshooting, the mass thresholds at the ZAMS for the formation of carbon–oxygen and oxygen–neon degenerate cores shift to smaller values by about 2 M⊙. As a by–product of our calculations, we have also obtained the structure and composition profiles of the resulting compact remnants. We find that the final fate of the considered stars could not be to become white dwarfs, as it is the case of objects of larger metallicity of analogous initial masses. Instead, as we show by means of a synthetic code, they might end their lives as SNI1/2.

  • Is there a chance for primordial SNI1/2?

     Gil Pons, Pilar
    Fisrt stars III
    Presentation's date: 2007-07-16
    Presentation of work at congresses

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  • Is there a chance for SNI1/2?

     Gil Pons, Pilar; Gutierrez Cabello, Jorge Luis; Garcia-berro Montilla, Enrique
    XXIII Trobades científiques de la Mediterrània: supernovae: light in the darkness
    p. 1-14
    Presentation of work at congresses

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  • On the fate of extremely low metallicity stars

     Gil Pons, Pilar; Gutierrez Cabello, Jorge Luis; Garcia-berro Montilla, Enrique; Althaus, Leandro Gabriel
    IXth Torino Workshop on Evolution and Nucleosynthesis in AGB Stars; II Perugia Workshop on Nuclear Astrophysics
    p. 71-78
    Presentation of work at congresses

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  • Is there a chance for primordial SNI1/2?

     Gil Pons, Pilar; Gutierrez Cabello, Jorge Luis; Garcia-berro Montilla, Enrique
    Fisrt stars III
    Presentation of work at congresses

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  • The First Nova explosions

     José Pont, Jordi; Garcia-berro Montilla, Enrique; Hernanz Carbó, Margarita; Gil Pons, Pilar
    The astrophysical journal letters
    Vol. 662, p. L103-L106
    Date of publication: 2007-06
    Journal article

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  • The Late stages of the evolution of intermediate-mass primordial stars: The effects of overshooting

     Gil Pons, Pilar; Gutierrez Cabello, Jorge Luis; Garcia-berro Montilla, Enrique
    Astronomy and astrophysics
    Vol. 464, num. 2, p. 667-682
    Date of publication: 2007-03
    Journal article

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  • The degenerate remnant cores of ultra-metal-poor heavy-weight intermediate-mass stars: white dwarfs of supernovae?

     Garcia-berro Montilla, Enrique; Gil Pons, Pilar; Gutierrez Cabello, Jorge Luis
    15th European Workshop on White Dwarfs
    p. 9-12
    Presentation of work at congresses

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  • The Degenerate remmant cores of ultra-metal-poor-heavy-weight intermediate mass stars: white dwarfs or supernovae?

     Garcia-berro Montilla, Enrique; Gil Pons, Pilar; Gutierrez Cabello, Jorge Luis
    15th European Workshop on White Dwarfs
    p. 9-12
    Presentation of work at congresses

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  • The Degenerate remmant cores of ultra-metal-poor-heavy-weight intermediate mass stars: white dwarfs or supernovae?

     Gil Pons, Pilar
    15th European Workshop on White Dwarfs
    Presentation's date: 2006-08-07
    Presentation of work at congresses

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  • The evolution of SAGB stars

     Gil Pons, Pilar
    VIII Torino Workshop on Nucleosynthesis in AGB stars
    Presentation's date: 2006-02-06
    Presentation of work at congresses

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  • The Evolution of primordial Super-AGB stars

     Garcia-berro Montilla, Enrique; Gil Pons, Pilar; Gutierrez Cabello, Jorge Luis
    Memorie della Societá Astronomica Italiana
    Vol. 77, num. 2, p. 834-839
    Date of publication: 2006-08
    Journal article

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  • Classical vs. primordial nova explosions

     José Pont, Jordi; Hernanz Carbó, Margarita; Garcia-berro Montilla, Enrique; Gil Pons, Pilar
    International Symposium on Nuclear Astrophysics - Nuclei in de Cosmos IX
    p. 1-5
    Presentation's date: 2006-06-25
    Presentation of work at congresses

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  • Ajuts de Recerca a Grups Consolidats de la Generalitat de Catalunya: Grup d'Astronomia i Astrofísica

     Garcia-berro Montilla, Enrique; Gil Pons, Pilar
    Competitive project

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  • The Formation of DA white dwarfs with thin hydrogen envelopes

     Althaus, Leandro Gabriel; Miller-Bertolami, M M; Córsico, A H; Garcia-berro Montilla, Enrique; Gil Pons, Pilar
    Astronomy and astrophysics
    Vol. 440, num. 1, p. L1-L4
    Date of publication: 2005-08
    Journal article

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  • Carbon burning in intermediate-mass primordial stars

     Gil Pons, Pilar; Suda, Takuma; Fujimoto, Masayuki Y.; Garcia-berro Montilla, Enrique
    Astronomy and astrophysics
    Vol. 433, num. 1, p. 1037-1046
    Date of publication: 2005-02
    Journal article

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  • On the frequency of ocurrence of novae hosting an ONe white dwarfs

     Gil Pons, Pilar; Garcia-berro Montilla, Enrique; José Pont, Jordi; Hernanz Carbó, Margarita; Truran, J W
    Astronomy and astrophysics
    Vol. 407, p. 1021-1028
    Date of publication: 2003-09
    Journal article

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  • On scenarios leading to symbiotic novae

     Gil Pons, Pilar; Garcia-berro Montilla, Enrique
    Date of publication: 2003-03
    Book chapter

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  • White dwarf population in the galactic halo (MCYT Plan de Astronomía, AYA2002-04094-C03-01)

     Garcia-berro Montilla, Enrique; Gil Pons, Pilar
    Competitive project

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  • ON THE EVOLUTION OF INTERMEDIATE MASS OBJECTS IN CLOSE BINARY SYSTEMS

     Gil Pons, Pilar
    Department of Applied Physics, Universitat Politècnica de Catalunya
    Theses

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  • The Impact of the chemical stratification of white dwarfs on the classification of classical novae

     José Pont, Jordi; Hernanz Carbó, Margarita; Garcia-berro Montilla, Enrique; Gil Pons, Pilar
    The astrophysical journal letters
    Vol. 597, p. L41-L44
    Date of publication: 2003-11
    Journal article

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  • The evolution of intermediate mass close binary systems: scenarios leading to novae

     Garcia-berro Montilla, Enrique; Gil Pons, Pilar
    Classical Novae Explosions
    p. 62-66
    Presentation of work at congresses

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  • The evolution of intermediate mass close binary systems: scenarios leading to novae

     Garcia-berro Montilla, Enrique; Gil Pons, Pilar
    International Conference on Classical Nova Explosions
    p. 10
    Presentation of work at congresses

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  • On scenarios leading to symbiotic novae

     Gil Pons, Pilar; Garcia-berro Montilla, Enrique
    Euroconference on Symbiotic Stars Probing Stellar Evolution
    p. 313-316
    Presentation of work at congresses

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  • On scenarios leading to symbiotic novae

     Gil Pons, Pilar
    Euroconference on Symbiotic Stars Probing Stellar Evolution
    Presentation's date: 2002-05-27
    Presentation of work at congresses

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  • Classical nova explosions: International conference on classical nova explosions, Sitges, Spain, 20-24 May, 2002

     Garcia-berro Montilla, Enrique; Gil Pons, Pilar; Truran, J W
    Date of publication: 2002-06
    Book

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  • On the formation of SAGB stars in intermediate mass close binary systems

     Gil Pons, Pilar; Garcia-berro Montilla, Enrique
    Astronomy and astrophysics
    Vol. 396, num. 2, p. 589-598
    Date of publication: 2002-12
    Journal article

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  • On the formation of oxygen neon white dwarfs in binary systems

     Gil Pons, Pilar; Garcia-berro Montilla, Enrique
    Date of publication: 2001-07
    Book chapter

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