THE QUASI-ROCHE LOBE OVERFLOW STATE IN THE EVOLUTION OF CLOSE BINARY SYSTEMS CONTAINING A RADIO PULSAR
We study the evolution of close binary systems formed by a normal (solar composition), intermediate-mass-donor star together with a neutron star. We consider models including irradiation feedback and evaporation. These nonstandard ingredients deeply modify the mass-transfer stages of these binaries....
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Published in | The Astrophysical journal Vol. 798; no. 1; pp. 1 - 8 |
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Format | Journal Article |
Language | English |
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01.01.2015
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Abstract | We study the evolution of close binary systems formed by a normal (solar composition), intermediate-mass-donor star together with a neutron star. We consider models including irradiation feedback and evaporation. These nonstandard ingredients deeply modify the mass-transfer stages of these binaries. While models that neglect irradiation feedback undergo continuous, long-standing mass-transfer episodes, models including these effects suffer a number of cycles of mass transfer and detachment. During mass transfer, the systems should reveal themselves as low-mass X-ray binaries (LMXBs), whereas when they are detached they behave as binary radio pulsars. We show that at these stages irradiated models are in a Roche lobe overflow (RLOF) state or in a quasi-RLOF state. Quasi-RLOF stars have radii slightly smaller than their Roche lobes. Remarkably, these conditions are attained for an orbital period as well as donor mass values in the range corresponding to a family of binary radio pulsars known as "redbacks." Thus, redback companions should be quasi-RLOF stars. We show that the characteristics of the redback system PSR J1723-2837 are accounted for by these models. In each mass-transfer cycle these systems should switch from LMXB to binary radio pulsar states with a timescale of approximately one million years. However, there is recent and fast growing evidence of systems switching on far shorter, human timescales. This should be related to instabilities in the accretion disk surrounding the neutron star and/or radio ejection, still to be included in the model having the quasi-RLOF state as a general condition. |
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AbstractList | We study the evolution of close binary systems formed by a normal (solar composition), intermediate-mass-donor star together with a neutron star. We consider models including irradiation feedback and evaporation. These nonstandard ingredients deeply modify the mass-transfer stages of these binaries. While models that neglect irradiation feedback undergo continuous, long-standing mass-transfer episodes, models including these effects suffer a number of cycles of mass transfer and detachment. During mass transfer, the systems should reveal themselves as low-mass X-ray binaries (LMXBs), whereas when they are detached they behave as binary radio pulsars. We show that at these stages irradiated models are in a Roche lobe overflow (RLOF) state or in a quasi-RLOF state. Quasi-RLOF stars have radii slightly smaller than their Roche lobes. Remarkably, these conditions are attained for an orbital period as well as donor mass values in the range corresponding to a family of binary radio pulsars known as ''redbacks''. Thus, redback companions should be quasi-RLOF stars. We show that the characteristics of the redback system PSR J1723-2837 are accounted for by these models. In each mass-transfer cycle these systems should switch from LMXB to binary radio pulsar states with a timescale of approximately one million years. However, there is recent and fast growing evidence of systems switching on far shorter, human timescales. This should be related to instabilities in the accretion disk surrounding the neutron star and/or radio ejection, still to be included in the model having the quasi-RLOF state as a general condition. |
Author | Benvenuto, O G De Vito, M A Horvath, J E |
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BackLink | https://www.osti.gov/biblio/22364729$$D View this record in Osti.gov |
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CitedBy_id | crossref_primary_10_1051_0004_6361_201628692 crossref_primary_10_1093_mnras_staa395 crossref_primary_10_1103_PhysRevD_102_043020 crossref_primary_10_1093_mnras_stv2607 crossref_primary_10_1142_S0218271823500463 crossref_primary_10_3847_1538_4357_ac8161 crossref_primary_10_1007_s11433_023_2247_x crossref_primary_10_1088_0004_637X_814_1_74 crossref_primary_10_1093_mnras_staa1304 crossref_primary_10_1088_0004_637X_809_1_99 crossref_primary_10_1017_S1743921318000480 crossref_primary_10_3847_1538_4357_aa9937 crossref_primary_10_3847_2041_8213_acfedf crossref_primary_10_3847_1538_4357_aac828 crossref_primary_10_3847_1538_4357_aaed43 crossref_primary_10_1093_mnras_stv990 crossref_primary_10_1093_mnras_stab2842 crossref_primary_10_3847_0004_637X_816_2_74 crossref_primary_10_1093_mnras_stv259 crossref_primary_10_1093_mnras_staa3072 crossref_primary_10_3847_1538_4357_aa5b7d |
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Snippet | We study the evolution of close binary systems formed by a normal (solar composition), intermediate-mass-donor star together with a neutron star. We consider... |
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SubjectTerms | ACCRETION DISKS APPROXIMATIONS ASTROPHYSICS, COSMOLOGY AND ASTRONOMY BINARY STARS EVAPORATION FEEDBACK IRRADIATION Lobes MASS TRANSFER NEUTRON STARS PULSARS Radio ROCHE EQUIPOTENTIALS STAR EVOLUTION STAR MODELS Stars Stellar system evolution X RADIATION |
Title | THE QUASI-ROCHE LOBE OVERFLOW STATE IN THE EVOLUTION OF CLOSE BINARY SYSTEMS CONTAINING A RADIO PULSAR |
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