The Expanding Bipolar Shell of the Helium Nova V445 Puppis

Woudt, P. A.; Steeghs, D.; Karovska, M.; Warner, Brian D.; Groot, P.; Nelemans, G.; Roelofs, G.; Marsh, T. R.; Nagayama, Takahiro; Smits, Derck P.; O’Brien, T. J.

doi:10.1088/0004-637x/706/1/738

Cited by 118 publications

(172 citation statements)

References 52 publications

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“…Wang & Han (2010c) suggested that the hot subdwarf HD 49798 and its X-ray pulsating companion could evolve into an SN Ia in the future. The system V445 Pup is another candidate of a massive WD + He star system, in which the mass of the WD is > ∼ 1.35 M , and the mass of the He star is > ∼ 0.85 M (Kato et al 2008;Woudt et al 2009). …”

Section: Discussion and Summarymentioning

confidence: 99%

Helium-star evolutionary channel to super-Chandrasekhar mass type Ia supernovae

Liu

Chen

Wang

et al. 2010

A&A

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The recent discovery of several overluminous type Ia supernovae (SNe Ia) indicates that the explosive masses of white dwarfs may significantly exceed the canonical Chandrasekhar-mass limit. Rapid differential rotation may support these massive white dwarfs (WDs). Based on the single-degenerate scenario and assuming that the WDs would differentially rotate when the accretion ratė M > 3 × 10 −7 M yr −1 , we performed the numerical calculations for ∼1000 binary systems consisting of a He star and a CO WD with Eggleton's stellar evolution code. We present the initial parameters in the orbital period − helium star-mass plane (for WD masses of 1.0 M and 1.2 M , respectively), which lead to super-Chandrasekhar mass SNe Ia. Our results indicate that for an initially massive WD of 1.2 M , a large number of SNe Ia may result from super-Chandrasekhar mass WDs. The highest mass of the WD at the moment of the SNe Ia explosion is 1.81 M , but very massive (>1.85 M ) WDs cannot be formed. However, when the initial mass of WDs is 1.0 M , the explosive masses of SNe Ia are nearly uniform, which is consistent with the rareness of super-Chandrasekhar mass SNe Ia in observations.

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Section: Discussion and Summarymentioning

confidence: 99%

Helium-star evolutionary channel to super-Chandrasekhar mass type Ia supernovae

Liu

Chen

Wang

et al. 2010

A&A

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“…Some recent examples suggest that bipolarity in the ejecta of classical/recurrent novae may be relatively frequent: RS Oph (Ribeiro et al 2009;Bode et al 2007;Chesneau et al 2007), V445 Pup (Woudt et al 2009), V1280 Sco (Chesneau et al 2008;Chesneau et al, in prep. ) or HR Del (Harman & O'Brien 2003).…”

Section: A Face-on Bipolar Eventmentioning

confidence: 99%

The 2011 outburst of the recurrent nova T Pyxidis. Evidence for a face-on bipolar ejection

Chesneau¹,

Meilland²,

Banerjee³

et al. 2011

A&A

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Aims. T Pyx is the first recurrent nova ever historically studied. It was seen in outburst six times between 1890 and 1966 and then not for 45 years. We report on near-IR interferometric observations of the recent outburst of 2011. Methods. We obtained near-IR observations of T Pyx at dates ranging from t = 2.37 d to t = 48.2 d after the outburst, with the CLASSIC recombiner located at the CHARA array and with the PIONIER and AMBER recombiners located at the VLTI array. These data are supplemented with near-IR photometry and spectra obtained at Mount Abu, India. We compare expansion of the H and K band continua and the Brγ emission line, and infer information on the kinematics and morphology of the early ejecta. Results. Slow expansion velocities were measured (≤300 km s −1 ) before t = 20 d. From t = 28 d on, the AMBER and PIONIER continuum visibilities (K and H band, respectively) are best simulated with a two-component model consisting of an unresolved source plus an extended source whose expansion velocity onto the sky plane is lower than ∼700 km s −1 . The expansion of the Brγ lineforming region, as inferred at t = 28 d and t = 35 d, is slightly larger, implying velocities in the range 500−800 km s −1 , which is still strikingly lower than the velocities of 1300−1600 km s −1 inferred from the Doppler width of the line. Moreover, a remarkable pattern was observed in the Brγ differential phases. A semi-quantitative model using a bipolar flow with a contrast of 2 between the pole and equator velocities, an inclination of i = 15• , and a position angle PA = 110• provides a good match to the AMBER observables. At t = 48 d, a PIONIER dataset confirms the two-component nature of the H band emission, consisting of an unresolved stellar source and an extended region whose appearance is circular and symmetric within error bars. Conclusions. These observations are most simply interpreted within the frame of a bipolar model, oriented nearly face-on. This finding has profound implications for interpreting past, current, and future observations of the expanding nebula.

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“…Helium overabundance is spectroscopically observed in some recurrent novae, U Sco (Williams et al 1981;Hanes 1985;Starrfield et al 1988) and V394 (Sekiguchi et al 1989), and some classical novae, Nova LMC 1990No. 2 (Sekiguchi et al 1990Shore et al 1991) and V445 Puppis (Nova Puppis 2000; Ashok & Banerjee 2003;Kato & Hachisu 2003;Kato et al 2008;Woudt et al 2009;Goranskij et al 2010). In most considerations in the literature, the helium-rich secondaries are the cores of stars stripped of their red giant envelopes by mass transfer (Iben & Tutukov 1994;Yoon & Langer 2003;Solheim & Yungelson 2005;Ruiter et al 2009Ruiter et al , 2011Wang et al 2009aWang et al , 2009bWang & Han 2009;Meng & Yang 2010).…”

Section: Discussionmentioning

confidence: 99%

Effects of Rotationally Induced Mixing in Compact Binary Systems With Low-Mass Secondaries and in Single Solar-Type Stars

Chatzopoulos¹,

Robinson²,

Wheeler³

2012

ApJ

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Many population synthesis and stellar evolution studies have addressed the evolution of close binary systems in which the primary is a compact remnant and the secondary is filling its Roche lobe, thus triggering mass transfer. Although tidal locking is expected in such systems, most studies have neglected the rotationally induced mixing that may occur. Here we study the possible effects of mixing in mass-losing stars for a range of secondary star masses and metallicities. We find that tidal locking can induce rotational mixing prior to contact and thus affect the evolution of the secondary star if the effects of the Spruit-Tayler dynamo are included both for angular momentum and chemical transport. Once contact is made, the effect of mass transfer tends to be more rapid than the evolutionary timescale, so the effects of mixing are no longer directly important, but the mass-transfer strips matter to inner layers that may have been affected by the mixing. These effects are enhanced for secondaries of 1-1.2 M and for lower metallicities. We discuss the possible implications for the paucity of carbon in the secondaries of the cataclysmic variable SS Cyg and the black hole candidate XTE J1118+480 and for the progenitor evolution of Type Ia supernovae. We also address the issue of the origin of blue straggler stars in globular and open clusters. We find that for models that include rotation consistent with that observed for some blue straggler stars, evolution is chemically homogeneous. This leads to tracks in the H-R diagram that are brighter and bluer than the non-rotating main-sequence turn-off point. Rotational mixing could thus be one of the factors that contribute to the formation of blue stragglers.

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The Expanding Bipolar Shell of the Helium Nova V445 Puppis

Cited by 118 publications

References 52 publications

Helium-star evolutionary channel to super-Chandrasekhar mass type Ia supernovae

Helium-star evolutionary channel to super-Chandrasekhar mass type Ia supernovae

The 2011 outburst of the recurrent nova T Pyxidis. Evidence for a face-on bipolar ejection

Effects of Rotationally Induced Mixing in Compact Binary Systems With Low-Mass Secondaries and in Single Solar-Type Stars

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