Modes of Mass Ejection by Binary Stars and the Effect on Their Orbital Periods.

Huang, Su-Shu

doi:10.1086/147659

Cited by 82 publications

(51 citation statements)

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“…For mass loss due to a direct fast stellar wind from the helium star (i.e. Jeans's mode, Huang 1963;van den Heuvel 1994), the orbital period change is given by:…”

Section: Fitting Formulae With Applications To Population Synthesismentioning

confidence: 99%

Ultra-stripped supernovae: progenitors and fate

Tauris¹,

Langer²,

Podsiadlowski³

2015

Monthly Notices of the Royal Astronomical Society

417

613

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The explosion of ultra-stripped stars in close binaries can lead to ejecta masses < 0.1 M ⊙ and may explain some of the recent discoveries of weak and fast optical transients. In Tau ris et al. (2013), it was demonstrated that helium star companions to neutron stars (NSs) may experience mass transfer and evolve into naked ∼ 1.5 M ⊙ metal cores, barely above the Chandrasekhar mass limit. Here we elaborate on this work and present a systematic investigation of the progenitor evolution leading to ultra-stripped supernovae (SNe). In particular, we examine the binary parameter space leading to electron-capture (EC SNe) and iron core-collapse SNe (Fe CCSNe), respectively, and determine the amount of helium ejected with applications to their observational classification as Type Ib or Type Ic. We mainly evolve systems where the SN progenitors are helium star donors of initial mass M He = 2.5 − 3.5 M ⊙ in tight binaries with orbital periods of P orb = 0.06 − 2.0 days, and hosting an accreting NS, but we also discuss the evolution of wider systems and of both more massive and lighter -as well as single -helium stars. In some cases we are able to follow the evolution until the onset of silicon burning, just a few days prior to the SN explosion. We find that ultra-stripped SNe are possible for both EC SNe and Fe CCSNe. EC SNe only occur for M He = 2.60 − 2.95 M ⊙ depending on P orb . The general outcome, however, is an Fe CCSN above this mass interval and an ONeMg or CO white dwarf for smaller masses. For the exploding stars, the amount of helium ejected is correlated with P orb -the tightest systems even having donors being stripped down to envelopes of less than 0.01 M ⊙ . We estimate the rise time of ultra-stripped SNe to be in the range 12 hr − 8 days, and light curve decay times between 1 and 50 days. A number of fitting formulae for our models are provided with applications to population synthesis. Ultrastripped SNe may produce NSs in the mass range 1.10 − 1.80 M ⊙ and are highly relevant for LIGO/VIRGO since most (possibly all) merging double NS systems have evolved through this phase. Finally, we discuss the low-velocity kicks which might be imparted on these resulting NSs at birth.

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“…For mass loss due to a direct fast stellar wind from the helium star (i.e. Jeans's mode, Huang 1963;van den Heuvel 1994), the orbital period change is given by:…”

Section: Fitting Formulae With Applications To Population Synthesismentioning

confidence: 99%

Ultra-stripped supernovae: progenitors and fate

Tauris¹,

Langer²,

Podsiadlowski³

2015

Monthly Notices of the Royal Astronomical Society

417

613

View full text Add to dashboard Cite

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“…from Huang (1963) paper, a relative mass transfer of m 2 /m 2 = 3.02 × 10 −7 yr −1 and hence the corresponding mass and angular momentum lost by secondary were obtained as m 2 = −8.80 × 10 −7 m sun /yr and J = −2.58 × 10 42 g cm 2 s −1 , respectively; where I have used the masses of the components given in Table 3 and (15) below from Applegate (1992).…”

Section: Mass Transfersmentioning

confidence: 99%

The O-C curve analysis and simultaneous light curve solutions of classical Algol system U Cephei

Manzoori

2008

Astrophys Space Sci

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New Photometric data in R and V passband filters of the classical Algol system U Cep were analyzed. The orbital and physical parameters of the system were obtained via light curve solutions, using Wilson-Devinney code. The absolute dimensions are also estimated. The O-C curve (only photometric data) is analyzed through Kalimeris method. Fourier analysis of P (E) function gave at least two modulation periods, i.e., P 1 = 16.38 yr and P 2 = 9.77 yr, the first was attributed to magnetic cycle effects and the second to mean time interval of occasional mass out bursts.

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“…Likewise, when the donor is the less massive star (w L1 > 0), the orbital period increases while the ΔT ( ) function is convex for any . Therefore, the foregoing analysis recovers the widely used procedure for estimating MT rates under conservative conditions in semi-detached and contact binaries (e.g., Kwee 1958;Huang 1963;Kruszewski 1964b). Given the ΔT ( ) function, Eq.…”

Section: Mass Transfer In the Absence Of An Accretion Diskmentioning

confidence: 74%

Efficiency of ETV diagrams as diagnostic tools for long-term period variations

Nanouris

Kalimeris

Antonopoulou

et al. 2015

A&A

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Context. The credibility of an eclipse timing variation (ETV) diagram analysis is investigated for various manifestations of the mass transfer and gravitational radiation processes in binary systems. The monotonicity of the period variations and the morphology of the respective ETV diagrams are thoroughly explored in both the direct impact and the accretion disk mode of mass transfer, accompanied by different types of mass and angular momentum losses (through a hot-spot emission from the gainer and via the L2/L3 points). Aims. Our primary objective concerns the traceability of each physical mechanism by means of an ETV diagram analysis. Also, possible critical mass ratio values are sought for those transfer modes that involve orbital angular momentum losses strong enough to dictate the secular period changes even when highly competitive mechanisms with the opposite direction act simultaneously. Methods. TheJ −Ṗ relation that governs the orbital evolution of a binary system is set to provide the exact solution for the period and the function expected to represent the subsequent eclipse timing variations. The angular momentum transport is parameterized through appropriate empirical relations, which are inferred from semi-analytical ballistic models. Then, we numerically determine the minimum temporal range over which a particular mechanism is rendered measurable, as well as the critical mass ratio values that signify monotonicity inversion in the period modulations. Results. Mass transfer rates comparable to or greater than 10 −8 M yr −1 are measurable for typical noise levels of the ETV diagrams, regardless of whether the process is conservative. However, the presence of a transient disk around the more massive component defines a critical mass ratio (q cr ≈ 0.83) above which the period turns out to decrease when still in the conservative regime, rendering the measurability of the anticipated variations a much more complicated task. The effects of gravitational radiation proved to be rather undetectable, except for systems with physical characteristics that only refer to cataclysmic variables. Conclusions. The monotonicity of the period variations and the curvature of the respective ETV diagrams depend strongly on the accretion mode and the degree of conservatism of the transfer process. Unlike the hot-spot effects, the Lagrangian points L2 and L3 support very efficient routes of strong angular momentum loss. It is further shown that escape of mass via the L3 point -when the donor is the less massive component -safely provides critical mass ratios above which the period is expected to decrease, no matter how intense the process is.

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Modes of Mass Ejection by Binary Stars and the Effect on Their Orbital Periods.

Cited by 82 publications

References 0 publications

Ultra-stripped supernovae: progenitors and fate

Ultra-stripped supernovae: progenitors and fate

The O-C curve analysis and simultaneous light curve solutions of classical Algol system U Cephei

Efficiency of ETV diagrams as diagnostic tools for long-term period variations

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