DOCSLIB.ORG

Structure of a Massive Common Envelope in the Common-Envelope Wind Model for Type Ia Supernovae

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Structure of a Massive Common Envelope in the Common-Envelope Wind Model for Type Ia Supernovae A&A 633, A41 (2020) Astronomy https://doi.org/10.1051/0004-6361/201936526 & c ESO 2020 Astrophysics Structure of a massive common envelope in the common-envelope wind model for Type Ia supernovae Ren Song1,2, Xiangcun Meng1,3,4 , Philipp Podsiadlowski5, and Yingzhen Cui1,2 1 National Astronomical Observatories/Yunnan Observatory, Chinese Academy of Sciences, Kunming 650216, PR China e-mail: [email protected], [email protected] 2 University of Chinese Academy of Sciences, Beijing 100049, PR China 3 Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, 650216 Kunming, PR China 4 Center for Astronomical Mega-Science, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing 100012, PR China 5 Department of Astronomy, Oxford University, Oxford OX1 3RH, UK Received 20 August 2019 / Accepted 13 November 2019 ABSTRACT Context. Although Type Ia supernovae (SNe Ia) are important in many astrophysical fields, the nature of their progenitors is still unclear. A new version of the single-degenerate model has been developed recently, the common-envelope wind (CEW) model, in which the binary is enshrouded in a common envelope (CE) during the main accretion phase. This model is still in development and has a number of open issues, for example what is the exact appearance of such a system during the CE phase? Aims. In this paper we investigate this question for a system with a massive CE. Methods. We use a thermally pulsing asymptotic giant branch (TPAGB) star with a CO core of 0.976 M and an envelope of 0.6 M to represent the binary system. The effects of the companion’s gravity and the rotation of the CE are mimicked by modifying the gravitational constant. The energy input from the friction between the binary and the CE is taken into account by an extra heating source. Results. For a thick envelope, the modified TPAGB star looks similar to a canonical TPAGB star but with a smaller radius, a higher effective temperature, and a higher surface luminosity. This is primarily caused by the effect of the companion’s gravity, which is the dominant factor in changing the envelope structure. The mixing length at the position of the companion can be larger than the local radius, implying a breakdown of mixing-length theory and suggesting the need for more turbulence in this region. The modified TPAGB star is more stable than the canonical TPAGB star and the CE density around the companion is significantly higher than that assumed in the original CEW model. Conclusions. Future work will require the modelling of systems with lower envelope masses and the inclusion of hydrodynamical effects during the CE phase. Key words. binaries: close – stars: evolution – supernovae: general – white dwarfs 1. Introduction involving the merging of two CO WDs (Tutukov & Yungelson 1981; Iben & Tutukov 1984; Webbink 1984). At present, both Type Ia supernovae (SNe Ia), some of the most violent explo- models have some theoretical and observational support. In this sions in the Universe, play an important role in a number of paper, we focus on a SD model. In the classical SD model, a astrophysical fields (Wang & Han 2012; Maoz et al. 2014). As CO WD accretes material from a non-degenerate companion star one of the best distance indicators, SNe Ia have been applied to increase its mass (Nomoto 1982). When the mass of the CO to measure cosmological parameters, which led to the discov- WD reaches a mass close to the Chandrasekhar limit, Mch, the ery of an accelerating expansion of the Universe (Riess et al. CO WD explodes as a SN Ia (Nomoto et al. 1984). In the SD 1998; Perlmutter et al. 1999). SNe Ia are also very important model, there is a critical accretion rate, M˙ cr. If the mass-transfer for the chemical evolution of galaxies as the main contributor of rate, M˙ tr, in the binary system exceeds M˙ cr, the WD expands iron neucleosynthesis (Matteucci & Greggio 1986). It is widely to form a RG-like object and then possibly swallows the com- believed that a SN Ia originates from the thermonuclear explo- panion to form a common envelope (CE, Nomoto 1982). The sion of a carbon-oxygen white dwarf (CO WD) in a binary sys- dynamics of the system during the CE phase are poorly under- tem (Hillebrandt et al. 2013), but the nature of the companion stood (Ivanova et al. 2013). The binary may lose its orbital angu- to the CO WD has remained controversial (Wang & Han 2012; lar momentum by friction with the CE and ultimately merge Maoz et al. 2014). rather than produce a SN Ia (Nomoto et al. 1979). On the other Depending on the companion’s nature, progenitor models of hand, if M˙ tr is too low, a nova explosion occurs and prevents the SNe Ia are mainly divided into two classes, the single-degenerate WD from gaining mass, again not leading to a SN Ia explosion (SD) model, in which the companion may be a main-sequence (Wang & Han 2012). Because of this fine-tuning, the birth rate (MS) star, a red giant (RG), or a helium star (Whelan & Iben of SNe Ia appears to be lower in the classical SD model than 1973;Nomoto et al.1984),andthedouble-degenerate(DD)model observed. Article published by EDP Sciences A41, page 1 of 10 A&A 633, A41 (2020) To increase the birth rate of SNe Ia in the SD model, Hachisu et al.(1996) developed the optically thick wind (OTW) model, which leads to a much higher SN Ia rate (Hachisu et al. 1999; Han & Podsiadlowski 2004), in fact comparable with the observed rate. In the OTW model, an OTW is assumed to occur when M˙ tr > M˙ cr, rather than the formation of a CE. The CO WD will then gradually increase its mass at the rate of M˙ cr and any unprocessed matter is blown off from the sur- face of the WD (Hachisu et al. 1996). However, some predic- tions from the OTW model are in conflict with observations. For example, because the OTW is driven by Fe lines, the OTW occurs only when Z ≥ 0:002, implying that there should be no SNe Ia in the early Universe or in low-metallicity environ- ments (Kobayashi et al. 1998). This cannot explain those SNe Ia that occur at high redshifts or in low-metallicity environments (Prieto et al. 2008; Rodney et al. 2015). In addition, the theoret- − ical OTW velocity (about 1000 km s 1, Hachisu et al. 1996) is Fig. 1. Schematic diagram illustrating the initial equivalent model dur- much higher than that inferred from observations of circumstel- ing the CE phase. The envelope is divided into three regions, the inner lar material (about 100 km s−1, Patat et al. 2007; Sternberg et al. co-rotating region (blue), the outer differentially rotating region (yel- 2011; Dilday et al. 2012). There are also some fine-tuning prob- low), and a transition region (light red) at the bottom of the outer region. lems in the OTW model, such as how to regulate simultane- The CO core represents the CO WD in the CEW model, in which stable hydrogen burning and helium shell flashes adjust themselves just as in ous (or alternating) helium and hydrogen burning (Piersanti et al. a normal TPAGB star. 2000; Shen & Bildsten 2007). To overcome the shortcomings of the OTW model, Meng & Podsiadlowski(2017; hereafter MP17) recently devel- 2. Numerical methods oped the common-envelope wind (CEW) model. In the CEW 2.1. Initial model model, when M˙ tr > M˙ cr a CE is assumed to form around the binary instead of an OTW. The CE is divided into two regions: In this study we use the Modules for Experiments in Stellar Astro- the inner region of the CE co-rotates with the binary, while the physics (MESA) code (version 10108; Paxton et al. 2011, 2013, outer region rotates differentially with the angular velocity drop- 2015, 2018) to carry out 1D hydrostatic simulations for systems ping off as a power law (following Meyer & Meyer-Hofmeister during the CE phase in the CEW model. As a first step in a series 1979). The CO WD increases its mass at the rate of M˙ cr. The of planned simulations, we simulate the structure of a binary sys- differentially rotating outer envelope extracts orbital angular tem with a massive CE as indicated by MP17. Because the system momentum from the inner binary into the outer region. Dur- is likely to look like a TPAGB star during the CE phase, we take a ing the CE phase, the system might look like a thermally puls- single TPAGB star as our starting model and simulate the effects of ing asymptotic giant branch (TPAGB) star in which alternating the spiraling-in companion in its envelope by changing the grav- phases of hydrogen and helium burning self-adjust just as they itational potential in the TPAGB star to imitate the effect of the do in TPAGB stars (MP17). The CEW model may resolve some companion’s gravity. This is a simple approximation, which we of the problems of the OTW model but also retain many of its discuss further in Sect.4. At present, three e ffects are considered: merits, such as only a weak dependence on the metallicity, and (1) the energy input from the secondary and the friction between the wind velocity from the CE surface is expected to be less than the binary system and the CE, (2) the gravity from the companion, about 200 km s−1, as inferred from observations.
Load more

Recommended publications
  • Luminous Blue Variables
    Review Luminous Blue Variables Kerstin Weis 1* and Dominik J. Bomans 1,2,3 1 Astronomical Institute, Faculty for Physics and Astronomy, Ruhr University Bochum, 44801 Bochum, Germany 2 Department Plasmas with Complex Interactions, Ruhr University Bochum, 44801 Bochum, Germany 3 Ruhr Astroparticle and Plasma Physics (RAPP) Center, 44801 Bochum, Germany Received: 29 October 2019; Accepted: 18 February 2020; Published: 29 February 2020 Abstract: Luminous Blue Variables are massive evolved stars, here we introduce this outstanding class of objects. Described are the specific characteristics, the evolutionary state and what they are connected to other phases and types of massive stars. Our current knowledge of LBVs is limited by the fact that in comparison to other stellar classes and phases only a few “true” LBVs are known. This results from the lack of a unique, fast and always reliable identification scheme for LBVs. It literally takes time to get a true classification of a LBV. In addition the short duration of the LBV phase makes it even harder to catch and identify a star as LBV. We summarize here what is known so far, give an overview of the LBV population and the list of LBV host galaxies. LBV are clearly an important and still not fully understood phase in the live of (very) massive stars, especially due to the large and time variable mass loss during the LBV phase. We like to emphasize again the problem how to clearly identify LBV and that there are more than just one type of LBVs: The giant eruption LBVs or h Car analogs and the S Dor cycle LBVs.
    [Show full text]
  • The Evolution of Luminous Red Nova at 2017Jfs in NGC 4470
    The evolution of luminous red nova AT 2017jfs in NGC 4470 Pastorello, A.; Chen, T. -W.; Cai, Y. -Z.; Morales-Garoffolo, A.; Cano, Z.; Mason, E.; Barsukova, E. A.; Benetti, S.; Berton, M.; Bose, S.; Bufano, F.; Callis, E.; Cannizzaro, G.; Cartier, R.; Chen, Ping; Dong, Subo; Dyrbye, S.; Elias-Rosa, N.; Floers, A.; Fraser, M.; Geier, S.; Goranskij, V. P.; Kann, D. A.; Kuncarayakti, H.; Onori, F.; Reguitti, A.; Reynolds, T.; Losada, I. R.; Carracedo, A. Sagues; Schweyer, T.; Smartt, S. J.; Tatarnikov, A. M.; Valeev, A. F.; Vogl, C.; Wevers, T.; de Ugarte Postigo, A.; Izzo, L.; Inserra, C.; Kankare, E.; Maguire, K.; Smith, K. W.; Stalder, B.; Tartaglia, L.; Thone, C. C.; Valerin, G.; Young, D. R. Published in: Astronomy & Astrophysics DOI: 10.1051/0004-6361/201935511 Publication date: 2019 Document version Publisher's PDF, also known as Version of record Document license: CC BY-NC Citation for published version (APA): Pastorello, A., Chen, T. -W., Cai, Y. -Z., Morales-Garoffolo, A., Cano, Z., Mason, E., Barsukova, E. A., Benetti, S., Berton, M., Bose, S., Bufano, F., Callis, E., Cannizzaro, G., Cartier, R., Chen, P., Dong, S., Dyrbye, S., Elias- Rosa, N., Floers, A., ... Young, D. R. (2019). The evolution of luminous red nova AT 2017jfs in NGC 4470. Astronomy & Astrophysics, 625, [L8]. https://doi.org/10.1051/0004-6361/201935511 Download date: 24. sep.. 2021 A&A 625, L8 (2019) Astronomy https://doi.org/10.1051/0004-6361/201935511 & c ESO 2019 Astrophysics LETTER TO THE EDITOR The evolution of luminous red nova AT 2017jfs in NGC 4470? A.
    [Show full text]
  • Formation of High-Field Magnetic White Dwarfs from Common Envelopes
    Formation of high-field magnetic white dwarfs from common envelopes Jason Nordhausa,1, Sarah Wellonsa, David S. Spiegela, Brian D. Metzgera, and Eric G. Blackmanb aDepartment of Astrophysical Sciences, Princeton University, Princeton, NJ 08544; and bDepartment of Physics and Astronomy, University of Rochester, Rochester, NY 14627 Edited by Neta A. Bahcall, Princeton University, Princeton, NJ, and approved January 12, 2011 (received for review October 6, 2010) The origin of highly magnetized white dwarfs has remained a mys- a nondegenerate companion), and SDSS has identified 149 tery since their initial discovery. Recent observations indicate that HFMWDs (none of which has a nondegenerate companion). the formation of high-field magnetic white dwarfs is intimately Assuming binomial statistics, the maximum probability of obtain- related to strong binary interactions during post-main-sequence ing samples at least this different from the same underlying −10 phases of stellar evolution. If a low-mass companion, such as a population is 5.7 × 10 , suggesting at the 6.2-σ level that the planet, brown dwarf, or low-mass star, is engulfed by a post-main- two populations are different (for details on this kind of calcula- sequence giant, gravitational torques in the envelope of the giant tion, see Appendix B of ref. 14). Furthermore, SDSS identified lead to a reduction of the companion’s orbit. Sufficiently low-mass 1,253 WD+M-dwarf binaries (none of which are magnetic). As companions in-spiral until they are shredded by the strong gravita- was previously pointed out, this suggests that the presence or tional tides near the white dwarf core.
    [Show full text]
  • Orihin and Evolution of Magnetars
    Origin and evolution of magnetars Sergei Popov (SAI MSU) (co-authors: A. Bogomazov, M. Prokhorov, R. Turolla) Plan of the talk • Origin of magnetars. Role of binaries • Evolution of magnetars. Binaries as probes. • Frozen magnetars in CCOs Origin of magnetars field Generated Fossil Critisized by Spruit (2008) Classical dynamo scenario starting from DT in 90s Dynamo mechanism conditions Rapid rotation is necessary! P0~ few msec This is difficult to achieve due to slowdown of a stellar core rotation (Heger et al. 2004, Meynet, Maeder 2005). The same problem appear in GRB scenario. Stellar rotation can be enhanced only in binaries. There are different possibilities to gain additional angular momentum due to mass transfer or tidal interaction. We need to to perform population synthesis calculations. Binary evolution channels. I. Among all possible evolutionary paths that result in formation of NSs we select those that lead to angular momentum increase of progenitors. • Coalescence prior to a NS formation. • Roche lobe overflow by a primary without a common envelope. • Roche lobe overflow by a primary with a common envelope. • Roche lobe overflow by a secondary without a common envelope. • Roche lobe overflow by a secondary with a common envelope. This is an optimistic scenarion, as it is assumed that angular momentum is not lost in significant amount after it has been gained (astro-ph/0505406) Products of binaries. I. In the “optimistic” scenario we obtain that rapidly rotating cores are mainly produced by mergers and by first RLO (i.e. the secondary companion gets angluar momentum). Mostly, compact objects formed via these channels are isolated.
    [Show full text]
  • Stellar Evolution
    AccessScience from McGraw-Hill Education Page 1 of 19 www.accessscience.com Stellar evolution Contributed by: James B. Kaler Publication year: 2014 The large-scale, systematic, and irreversible changes over time of the structure and composition of a star. Types of stars Dozens of different types of stars populate the Milky Way Galaxy. The most common are main-sequence dwarfs like the Sun that fuse hydrogen into helium within their cores (the core of the Sun occupies about half its mass). Dwarfs run the full gamut of stellar masses, from perhaps as much as 200 solar masses (200 M,⊙) down to the minimum of 0.075 solar mass (beneath which the full proton-proton chain does not operate). They occupy the spectral sequence from class O (maximum effective temperature nearly 50,000 K or 90,000◦F, maximum luminosity 5 × 10,6 solar), through classes B, A, F, G, K, and M, to the new class L (2400 K or 3860◦F and under, typical luminosity below 10,−4 solar). Within the main sequence, they break into two broad groups, those under 1.3 solar masses (class F5), whose luminosities derive from the proton-proton chain, and higher-mass stars that are supported principally by the carbon cycle. Below the end of the main sequence (masses less than 0.075 M,⊙) lie the brown dwarfs that occupy half of class L and all of class T (the latter under 1400 K or 2060◦F). These shine both from gravitational energy and from fusion of their natural deuterium. Their low-mass limit is unknown.
    [Show full text]
  • The Evolution of Close Binaries
    The Evolution of Close Binaries Philipp Podsiadlowski (Oxford) The case of RS Ophiuchi • as a test of binary stellar evolution • as a potential Type Ia supernova (SN Ia) progenitor I. Testing Binary Evolution: the Case of sdB Stars II. Problems in Binary Evolution III. The Progenitors of SNe Ia III. The Origin of Symbiotic Binaries IV. The Status of RS Ophiuchi Testing Binary Evolution: sdB Stars (Han et al. 2002, 2003) • sdB stars are helium-core-burning stars (with M ' 0.5 M ) that have lost most of their envelopes by binary interactions • prototypical evolution for forming compact bina- ries . stable Roche-lobe overflow . common-envelope (CE) evolution . binary mergers • all channels appear to be important (∼> 50% are short-period, post-CE binaries; Maxted, Heber, Napiwotzki) • mass transfer must have started near the tip of the red-giant branch (helium burning!) → ideal systems to test/constrain binary evolution Common−Envelope Channels stable RLOF + CE (mass ratio < 1.2 − 1.5) CE only (mass ratio > 1.2 − 1.5) Stable RLOF Channel stable RLOF (mass ratio < 1.2 − 1.5) stable RLOF (near tip of RGB) wide binary He WD MS unstable RLOF −−−> dynamical mass transfer unstable RLOF −−−> dynamical mass transfer wide sdB binary with MS/SG companion common−envelope phase common−envelope phase He He He MS P = 10 − 500 days orb M = 0.30 − 0.49 M sdB sun short−period sdB binary with He WD companion short−period sdB binary with MS companion P = 0.1 − 10 days orb M = 0.4 − 0.49 M sdB sun Problems in Binary Evolution (Selection) Common-envelope evolution and The criterion for dynamical mass transfer ejection • dynamical mass transfer is caused by a • dynamical mass transfer leads to a mass-transfer runaway (giant expands, CE and spiral-in phase Roche lobe shrinks) = • if envelope is ejected → short-period .
    [Show full text]
  • Luminous Red Nova Phenomenon
    Stars: from Collapse to Collapse ASP Conference Series, Vol. 510 Yu. Yu. Balega, D. O. Kudryavtsev, I. I. Romanyuk, and I. A. Yakunin, eds. c 2017 Astronomical Society of the Pacific Luminous Red Nova Phenomenon E. A. Barsukova 1, V. P. Goranskij 2, and A. F. Valeev 1 1Special Astrophysical Observatory of the Russian Academy of Sciences, Nizhnii Arkhyz, Russia 2Sternberg Astronomical Institute, Lomonosov Moscow State University, Russia Abstract. Luminous red novae form a new type of variable stars which explode turning into cool supergiants. We present a review of the main physical properties of the objects of this class. Most of them are mergers in close binary systems, but some of them may have a di fferent nature. Luminous red novae (LRN) are the stars erupting into cool supergiants (Munari et al. 2002). In other words, they are the stars with cool explosions. Along with the giant eruptions of massive stars, such as the Great eruption of η Car, they form a new class called ILOTs, namely, Intermediate Luminosity Optical Transients. At the outburst maximum, such stars become the brightest in their galaxies, only supernovae exceeded them by luminosity. At maximum, red novae have a definitely red color, K–M spectra of supergiants, evolving to more and more later spectral subclass, and they don’t pass a nebular phase characteristic of classical novae. Great interest to red novae is attracted by the assumption on their origin as a result of merging in close binary systems. In a unique case for the first time, merging process in a contact binary system was observed directly.
    [Show full text]
  • Common Envelope Evolution
    Planetary Nebulae, An Eye to the Future Proceedings IAU Symposium No. 283, 2011 c 2011 International Astronomical Union DOI: 00.0000/X000000000000000X Common Envelope Evolution Robert G. Izzard1, Philip D. Hall2, Thomas M. Tauris1,3 and Christopher A. Tout2 1Argelander-Insitut f¨ur Astronomie, Universit¨at Bonn, Auf dem H¨ugel 71, 53121 Bonn, Germany 2Institute of Astronomy, The Observatories, Madingley Road, Cambridge CB3 0HA, United Kingdom 3Max-Plack-Insitut f¨ur Radioastronomie, Auf dem H¨ugel 69, 53121 Bonn, Germany Abstract. Many binary star systems are not wide enough to contain the progenitor stars from which they were made. One explanation for this is that when one star becomes a red giant a common envelope forms around both stars in the binary system. The core of the giant and its companion star continue to orbit one another inside the envelope. Frictional energy deposited into the common envelope may lead to its ejection and, if so, a close binary system is formed from the core of the former giant star and its relatively untouched companion. When the primary is an asymptotic giant branch star the core becomes a hot carbon-oxygen white dwarf which may ionise the ejected envelope and illuminate a planetary nebula. Many other types of binary systems form through common envelope evolution such as low-mass X-ray binaries and cataclysmic variables. In the case of a failed envelope ejection when the cores merge, rapidly-rotating solitary giants similar to FK Comae stars form. In this short review we focus on attempts to constrain parameters of common envelope evolution models and also describe the latest efforts to model this elusive phase of binary stellar evolution.
    [Show full text]
  • How to Find Stellar Black Holes? (Notes)
    How to find stellar black holes? (Notes) S. R. Kulkarni December 5, 2018{January 1, 2019 c S. R. Kulkarni i Preface This are notes I developed whilst teaching a mini-course on \How to find (stellar) black holes?" at the Tokyo Institute of Technology, Japan during the period December 2018{February 2019. This was a pedagogical course and not an advanced research course. Every week, over a one and half hour session, I reviewed a different technique for finding black holes. Each technique is mapped to a chapter. The student should be aware that I am not an expert in black holes, stellar or otherwise. In fact, along with my student Helen Johnston, I have written precisely one paper on black holes, almost three decades ago. So, I am as much a student as a young person starting his/her PhD. This explains the rather elementary nature of these notes. Hopefully, it will be useful introduction and guide for future students interested in this topic. S. R. Kulkarni Ookayama, Ota ku, Tokyo, Japan Chance favors the prepared mind. • The greatest derangement of the mind is to believe in something because one wishes• it to be so { L. Pasteur We have a habit in writing articles published in scientific journals to make the work• as finished as possible, to cover all the tracks, to not worry about the blind alleys or to describe how you had the wrong idea first, and so on. So there isn't any place to publish, in a dignified manner, what you actually did in order to get to do the work.
    [Show full text]
  • Binary Black Hole Mergers: Formation and Populations
    MINI REVIEW published: 09 July 2020 doi: 10.3389/fspas.2020.00038 Binary Black Hole Mergers: Formation and Populations Michela Mapelli 1,2,3* 1 Physics and Astronomy Department Galileo Galilei, University of Padova, Padova, Italy, 2 INFN–Padova, Padova, Italy, 3 INAF–Osservatorio Astronomico di Padova, Padova, Italy We review the main physical processes that lead to the formation of stellar binary black holes (BBHs) and to their merger. BBHs can form from the isolated evolution of massive binary stars. The physics of core-collapse supernovae and the process of common envelope are two of the main sources of uncertainty about this formation channel. Alternatively, two black holes can form a binary by dynamical encounters in a dense star cluster. The dynamical formation channel leaves several imprints on the mass, spin and orbital properties of BBHs. Keywords: stars: black holes, black hole physics, Galaxy: open clusters and associations: general, stars: kinematics and dynamics, gravitational waves 1. BLACK HOLE FORMATION FROM SINGLE STARS: WHERE WE STAND NOW About 4 years ago, the LIGO detectors obtained the first direct detection of gravitational waves, Edited by: GW150914 (Abbott et al., 2016; Abbott et al., 2016a,b), associated with the merger of two black holes Rosalba Perna, (BHs). This event marks the dawn of gravitational wave astronomy: we now know that binary black Stony Brook University, United States holes (BBHs) exist, can reach coalescence by gravitational wave emission, and are composed of BHs ∼ Reviewed by: with mass ranging from few solar masses to 50 M⊙. Here, we review the main physical processes Maxim Yurievich Khlopov, that lead to the formation of BBHs and to their merger.
    [Show full text]
  • Pos(Texas 2010)085 Ni Is Expected to Be Produced This 56 G, and Can Destroy the Entire Companion If It Is As Strong 15 Erg
    Recycling of Neutron Stars in Common Envelopes: A New Mechanism of Hypernovae Explosions. PoS(Texas 2010)085 M.V. Barkov Max-Planck-Institut für Kernphysik, Saupfercheckweg 1, D-6917 Heidelberg, Germany Space Research Institute, 84/32 Profsoyuznaya Street, Moscow,Russia Department of Applied Mathematics, The University of Leeds, Leeds, LS2 9JT, UK E-mail: [email protected] S.S. Komissarov Department of Applied Mathematics, The University of Leeds, Leeds, LS2 9JT, UK E-mail: [email protected] In this paper we propose a new plausible mechanism of supernova explosions specific to close binary systems. The starting point is the common envelope phase in the evolution of a binary consisting of a red super giant and a neutron star. As the neutron star spirals towards the center of its companion it spins up via disk accretion. Depending on the specific angular momentum of gas captured by the neutron star via the Bondi-Hoyle mechanism, it may reach millisecond periods either when it is still inside the common envelope or after it has merged with the companion core. The high accretion rate may result in strong differential rotation of the neutron star and generation of the magnetar-strength magnetic field. The magnetar wind can blow away the common envelope if its magnetic field is as strong as 1015 G, and can destroy the entire companion if it is as strong as 1016 G. The total explosion energy can be comparable to the rotational energy of a millisecond pulsar and reach 1052 erg. However, only a small amount of 56Ni is expected to be produced this way.
    [Show full text]
  • Blue Supergiant Progenitor Models of Type II Supernovae
    A&A 552, A105 (2013) Astronomy DOI: 10.1051/0004-6361/201321072 & c ESO 2013 Astrophysics Blue supergiant progenitor models of type II supernovae D. Vanbeveren, N. Mennekens, W. Van Rensbergen, and C. De Loore Astrophysical Institute, Vrije Universiteit Brussel, Pleinlaan 2, 1050 Brussels, Belgium e-mail: [email protected] Received 9 January 2013 / Accepted 6 March 2013 ABSTRACT We show that within all the uncertainties that govern the process of Roche-lobe overflow in case Br-type massive binaries, it cannot be excluded that a significant fraction of them merge and become single stars. We demonstrate that at least some of them will spend most of their core helium-burning phase as hydrogen-rich blue stars, populating the massive blue supergiant region and/or the massive Be-type star population. The evolutionary simulations lead us to suspect that these mergers will explode as luminous blue hydrogen- rich stars, and it is tempting to link them to at least some superluminous supernovae. Key words. binaries: close – stars: massive – supernovae: general – stars: evolution 1. Introduction 2. Evolution scenarios of blue progenitors of type II supernovae: a review Most type II supernova progenitors are red supergiants, but SN 1987A in the Large Magellanic Cloud provided strong ev- 2.1. Single-star progenitor models of SN 1987A idence that the progenitor of a type II supernova can also be a massive hydrogen-rich blue supergiant with a mass ∼20 M Langer (1991) investigated the effect of semiconvection on the (Arnett et al. 1989). evolution of massive single stars with initial mass between 7 M Since the discovery in 1999 of the first superluminous and 32 M and with metallicity Z = 0.005.
    [Show full text]