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

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PoS(Texas 2010)085 http://pos.sissa.it/ Ni is expected to be produced this 56 G, and can destroy the entire companion if it is as strong 15 erg. However, only a small amount of 52 G. The total explosion energy can be comparable to the rotational energy of a millisecond 16 [email protected] [email protected] way. The result isphase, an followed unusual by a type-II sharp supernova dropa with in solitary very brightness high magnetar and a luminosity or steep during aWolf-Rayet light-curve star the close tail. explodes plateau this binary The will involving remnant be a is a third either Wolf-Rayet supernovae star explosion in and the a same magnetar. binary. When this pulsar and reach 10 In this paper we proposebinary a systems. new plausible The mechanism starting ofconsisting point of supernova is a explosions red the specific super common giant to and envelopeits close a companion phase neutron it in star. spins As up the the via evolution neutron diskcaptured star of accretion. spirals by a Depending towards the on the binary the neutron center specific of star angulareither via momentum when of the it gas Bondi-Hoyle is still mechanism, inside it theThe may common high envelope reach accretion or rate millisecond after may it periods result has in mergedof strong with the differential magnetar-strength the rotation magnetic companion of field. the core. The neutron magnetar star windif and can generation its blow magnetic away the field common is envelope asas strong 10 as 10 Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-ShareAlike Licence. c

25th Texas Symposium on Relativistic AstrophysicsDecember - 06-10, TEXAS 2010 2010 Heidelberg, Germany S.S. Komissarov Department of Applied Mathematics, The UniversityE-mail: of Leeds, Leeds, LS2 9JT, UK M.V. Barkov Max-Planck-Institut für Kernphysik, Saupfercheckweg 1, D-6917Space Heidelberg, Germany Research Institute, 84/32 Profsoyuznaya Street,Department Moscow,Russia of Applied Mathematics, The UniversityE-mail: of Leeds, Leeds, LS2 9JT, UK Recycling of Neutron Stars in CommonA Envelopes: New Mechanism of Hypernovae Explosions. PoS(Texas 2010)085 (2.1) (2.2) (2.3) (2.4) ]. The heating of 3 ]; and the rotational 1 3, the accretion flow becomes / 4 . 3 = ) γ ∗ M , M ∞ , ( , v 2 A ]. It is rather feasible that the gravitational 4 ∗ ∞ R 2 ]: the strongly disturbed outer layers rapidly β ρ M aM 4 Ω 2 2 A 4 β η R η 2 2 a π = ≈ ≈ = i A A 2 760 Hz [ j i R B-H h A ˙ ∼ j GM M h ]. Only if the accretion proceeds at the Bondi-Hoyle rate the = 7 c , R 6 , for the polytropic index , A 5 R 25 . 0 = acc R the accretion on NS may proceed in more or less spherical fasion as in the Bondi c accretion radius R 8 and only weakly depends on model of RSG. A . 0 R is a free parameter, which reflects our current ignorance. ' R η β where We will assume that Given the specific angular momentum we can estimate at what radius from NS the Bondi- For The Bondi-Hoyle mass accretion rate is well approximated by the equation As the neutron spirals inside its giant companion it accretes mass and angular momentum. The The observations of fast rotating NS suggest a presence of a limiting value for the rotation pe- ] proposed this scenario as an alternative interpretation of long GRBs. 4 where where Hoyle trapped gas will form an accretion disk, solution, where at loose their angular momentum via gravitational radiation,and this generation leads of to a magnetar strong strength differentialfied magnetic rotation magnetic field field in becomes the unstablea stellar to powerful interior. the magnetically buoyancy Eventually, driven instability this pulsar-like andThis ampli- wind emerges scenario rapidly on provides extracts an the efficient the surface, way rotational and [ to energy realize of the rotation the power star. to the explosion. In particular, accretion can proceed at the Eddingtongenerated rate or during at the the much collision higher ofin Bondi-Hoyle the accreted rate if accretion matter the flow. with radiation This NSefficiency of depends or neutrino on its cooling the accretion [ position diskrecycling of of becomes the NS trapped accretion is sufficiently shock, fast which and depends the explosion of can the occure. 2. Inspiral dynamics and recycling of NS riod: the fastest known millisecond radio pulsar has the frequency of 641 Hz [ Recycling of Neutron Stars in Common Envelopes 1. Introduction radiation losses posse such awhere limit. its Indeed, r-mode as oscillation the is rotation excitedNS, spin associated via grows with the the the emission oscillations, star of reduces may gravitationallayers. the enter waves viscosity [ a This and regime decouples may its result interior from in the a outer magnetic explosion [ frequency of the fastest X-ray pulsar is supersonic. Its collision withwave, the which may NS not surface effect the or mass the accretion surface rate of provided two its conditions accretion are satisfied. disk creates a shock PoS(Texas 2010)085 .

M after (2.5) (2.6) (2.7) 8 and 25 / for the Ω 1 , = 4 η / rsg 1 , M 2 / 1 , ] for 1 8 = η

. M 1 ) − 1 yr − P

yr 1ms . M

( 8 4 2 η M few intermediate values of ) ) 08 ∝ . cn2 1 c cm cn2 6 R R M ) parameter are shown: ˙ M 10km 10 η c cm ( 6 R 7 14 . )( 2 10 3 and

− ( M ) 3 M 5 13.5 . − 16 . 1 2 cm acc 10 8 η ( R 13 × 10 has to exceed the critical value ∝ , Figure 1 shows 27 1 . . ( η 0 exceeds the critical value cn1 1 B-H 4 ˙ ˙ 12.5 M ' M ≈ BH 10 ˙ I K M cn1 j ≈ Ω R ˙ 12 M 10 cn2 ' ˙ log M M 11.5 ∆ 11 . If it does the radiation pressure prevents the mass accretion rate to exceed the A is very sensitive to R cn2 10.5 M Accretion rate as a function of the distance between the RSG center and NS (we note that NS is ac- 10 4. , / 1 Firstly, the radiation produced by the gas heated at the accretion shock should not be able to Secondly, the shock has to be inside the sonic surface of the Bondi ﬂow. Otherwise, the shock Since Once the accretion disk is formed the speciﬁc angular momentum of the gas settling on the NS 2 0 6 4 8

10 12 −2 −4

10 sun

dM/dt (M dM/dt log )

yr 16. For these values, the interaction of the NS with the envelop prevents an efficient accretion to the NS, . −1 / escape beyond unless the Bondi-Hoyle rate, which is shownaccretion by rates, the the thick accretion solid occurs line, at exceeds the the critical Bondi-Hoyle value. regime. For the higher Edington rate. For this to occure 1 The critical accretion rates for the following values of the cannot be a part of thecondition stationary is solution satisfied and when hence the the Bondi-type accretion is not realised. This As we shall see this conditioneter is more restrictive. The critical rates are quite sensitive to the param- model RSG25. One can see the fast accretion regime (at Bondi-Hoyle rates) is only possible when surface is that of the lastaccumulating Keplerian orbit. In this case the star will reach the rotational rate η commodated by the RSG star) as obtained in the frameworks of the model suggested by [ Figure 1: Recycling of Neutron Stars in Common Envelopes PoS(Texas 2010)085 15 by c 10 R × 3 = B 14 4 13.5 13 1. The orbital radius is shown by the solid line, the sonic point, . 0 = 12.5 η 12 R cm 10 log parameter 11.5 η 11 10.5 The distribution of the density (left panel) and the angular dependence of the energy flux at the The illustration to the typical linear scales of the scenario as function of the distance between the 10 9 8 7 6

11 10 14 13 12 , by the dotted line, the accretion shock radius by the dashed line, and the circularization radius,

i 10

cm r log acc G (see the contour lines inseen that the the left expected panel). released The energy velocity flux map is is strongly shown anisotropic. by arrows in the left panel. It may be the dash-doted line. Figure 3: distance of 110 km (right panel)The initial are density shown was for uniform, the and moment the 0.056 magnetic s field was after assumed the to magnetically be driven a explosion. shifted dipole field Figure 2: RSG center and NS. Thea calculations specific are value performed of in the the frameworks of the same model as in Fig. 1 for R Recycling of Neutron Stars in Common Envelopes PoS(Texas 2010)085 th (3.1) (3.2) at pre- , Nature 3 the shock − 1, when the sh v > . During the CE 10 1 erg cm R − 27 yr ] which is an alterna-

9 ]). A detailed numerical M 1 13 A millisecond pulsar , ∼ 12 2 1 − 10 − R 1 − , 1 and can reach 10 km s − sh v 3 52 − , 48 L tot E 17 ]. In a close binary system formed by a normal 10 erg cm 370 5 10 × ≈ 19 8 c ≈ NS tot 3 is distance between NS and center of RSG, E R M Lt R . We can see that the pressure in the bubble is smaller than 3 π 3 c 4 ≤ ], we can explain the big amount of hydrogen in the external ≈ , here 11 kick sh v bub v P / R , the binary system cannot be destroyed, since the outer envelop does ≈ NS ergs. t M 52 10 / tot E = 52 (1982), 615–618. , tot 300 E One of the important details in this model is that the explosion occurs strongly non-central, We note that the magnetic field topology is very important. Since the dynamo mechanism Our model suggest an interpretation of anomalously bright SN2006gy [ In the case of the remote explosion, although the mass of the RSG envelop can be bigger than ]. In this way, an ideal configuration for the explanation of anomalously bright SN is formed. In [1] D. C. Backer, S. R. Kulkarni, C. Heiles, M. M. Davis, and W. M. Goss, 4 simulations display two side jetenergy ratio configurations is but close with to 2:1 significantly –see different Fig.3–). power This in allows to jets estimate (the the kick for NS as References for the following epoch here supernovae stage, thus the pressure in the bubble could be estimated as wave speed in the speed ofthe light pressure units in the center of RSG, unless the explosion occurs at the distance of when NS is recycledpressure till in the the limiting center frequencies of before RSG reaching is the order center of of 10 RSG star. The can generate multiples configurations, aexpected superposition to of produce dipole a and shifted quadrupolefeatures dipole magnetic since field field it configuration. is should Therealize automatically shifted (another examples dipole lead of model one to side has an jets important one unsymmetrical can find explosion in and the works one [ side energy the frameworks of our scenarioenvelop [ and anomaly intensive stellar wind. not influence gravitationally on bounded system of NS + C/O core. mass of C/O core and Recycling of Neutron Stars in Common Envelopes 3. Discussion tive to the pulsation pair instabilitystar supernovae and [ NS, the normal starLagrangian point. in the When the stage NS of approaches Rochecan too expect lobe close, a overflow, the produces very CE dense a stage stellar strong has wind wind to with from begin. mass 1 At loss this rate epoch at we the level of shock wave cannot destroy the stellar C/Othe core. whole If RSG the can explosion occurs be in destroyed the by stellar the center explosion. vicinity, stage the fast accretion toovertake NS the leads stability to limit a andof GW recycling NS radiation of slowdown can the its start NS rotation to up[ and be to a very ms strong efficient. periods. magnetic Thus, field This the could rotation outer be can layers generated in the vicinity of NS PoS(Texas 2010)085 376 401 , ApJ (1996), 322–+. , MNRAS 459 , ApJ One-sided Outflows/Jets (1993), L33–L36. 411 (2007), 1116–1128. (1999), L1–L4. 666 341 , ApJ , Stellar Rotation (A. Maeder & P. Eenens, , ApJ Presupernova Evolution of Rotating Massive , A&A , ArXiv e-prints (2010). 6 Carinae η Pulsational pair instability as an explanation for the most Recycling of Neutron Stars in Common Envelopes and Close binary progenitors of gamma-ray bursts Black holes, white dwarfs, and neutron stars: The physics of (2007), 390–392. Steady spherical hypercritical accretion onto neutron stars 450 (2003), 42–44. Nuclear-powered millisecond pulsars and the maximum spin frequency of , ArXiv: 1012.4565 (2010) accepted by MNRAS. 424 , Nature Neutron star accretion in a stellar envelope SN 2006gy: Discovery of the Most Luminous Supernova Ever Recorded, Powered by , 1983. Gamma-ray bursts from X-ray binaries , Nature Neutrino-cooled Accretion: Rotation and Stellar Equation of State , from Rotating Stars with Complex Magnetic Fields Hypernova Explosions the Death of an Extremely Massive Star like luminous supernovae (2010), 1644–1656. neutron stars Stars and the Rotation Rate ofed.), Pulsars IAU (Invited Symposium, Review) vol. 215, June 2004, pp. 591–+. compact objects (1991), 234–244. [9] N. Smith, et al., [7] [8] A. Heger, S. E. Woosley, N. Langer, and H. C. Spruit, [4] H. C. Spruit, [5] J. C. Houck and R. A. Chevalier, [6] R. A. Chevalier, [2] D. Chakrabarty, et al., [3] S. L. Shapiro and S. A. Teukolsky, [11] M. V. Barkov and S. S. Komissarov, [12] M. V. Barkov and S. S. Komissarov, [13] R. V. E. Lovelace, M. M. Romanova, G. V. Ustyugova, and A. V. Koldoba, [10] S. E. Woosley, S. Blinnikov, and A. Heger, Recycling of Neutron Stars in Common Envelopes