Y. Tuchman

Hebrew University of Jerusalem

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J. C. Wheeler

The University of Texas at Austin

Z. Barkat

Hebrew University of Jerusalem

N. Sack

Hebrew University of Jerusalem

E. Livne

Hebrew University of Jerusalem

A. Yaari

Hebrew University of Jerusalem

M. O. Mennessier

Centre National de la Recherche Scientifique

S. M. Asida

University of Chicago

D. Barthés

Universitat de Barcelona

Shin Mineshige

Kyoto University

J. A. Mattei

American Association of Variable Star Observers

Cooperative Institutions

University of California, Santa Cruz

Universitätsmedizin Göttingen

Hebrew University of Jerusalem

University of California, Berkeley

Goddard Space Flight Center

Czech Academy of Sciences, Institute of Physics

Centre National de la Recherche Scientifique

Max Planck Institute for Astrophysics

Lawrence Berkeley National Laboratory

Lawrence Livermore National Laboratory

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Mass loss from dynamically unstable stellar envelopes

The Astrophysical Journal (1978)

Y. Tuchman N. Sack Z. Barkat

view Abstract Citations (85) References (26) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS Mass loss from dynamically unstable stellar envelopes. Tuchman, Y. ; Sack, N. ; Barkat, Z. Abstract Results of an extensive study of the dynamical stability and dynamical behavior of envelopes of red giants are given. The region on the luminosity-effective temperature plane within which static, thermally equilibrated envelopes are dynamically unstable is reanalyzed and is found to be more complex than has hitherto been thought. The significance of the structure of this region and its dependence on relevant physical parameters is discussed. The motion of unstable envelopes is followed by a numerical hydrodynamical code; it is found that some small amount of mass loss occurs via a shock ejection mechanism as previously suggested in the literature. It is, however, also found that this mass loss does occur repeatedly, so that a rather large amount of mass loss is expected over an evolutionary time scale. Publication: The Astrophysical Journal Pub Date: January 1978 DOI: 10.1086/155767 Bibcode: 1978ApJ...219..183T Keywords: Dynamic Stability; Hydrodynamics; Red Giant Stars; Stellar Envelopes; Stellar Mass Ejection; Stellar Models; Late Stars; Stellar Evolution; Stellar Luminosity; Stellar Temperature; Astrophysics; Envelopes:Red Giants; Mass Loss:Red Giants full text sources ADS |

Stellar mass

Stellar physics

10.1086/155767

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Citations (50)

Confrontation between power spectra of Mira stars and theoretical models.

Astronomy and Astrophysics (1994)

D. Barthés Y. Tuchman

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Pb208(p,d)Pb

Physical Review C (1974)

E. Friedman D. Nir D. Suraqui Y. Tuchman

The $^{208}\mathrm{Pb}(p,d)^{207}\mathrm{Pb}$ reaction to the $3{p}_{\frac{1}{2}}$, $2{f}_{\frac{5}{2}}$, and $3{p}_{\frac{3}{2}}$ single-hole states was studied at energies below the Coulomb barrier. The $^{48}\mathrm{Ca}(d,t)^{47}\mathrm{Ca}$ reaction to the $1{f}_{\frac{7}{2}}$ single-hole state was studied near the Coulomb barrier. Distorted-wave Born-approximation analyses provided values for the root-mean-square radii of the orbitals of the picked-up neutrons. These values are in agreement with results obtained from other reactions and from nuclear-structure calculations, but disagree with values based on analyses of Coulomb displacement energies.[NUCLEAR REACTIONS $^{208}\mathrm{Pb}(p,d)$, $E=12$ MeV; measured $\ensuremath{\sigma}({E}_{d},\ensuremath{\theta})$. $^{48}\mathrm{Ca}(d,{t}_{0})$, $E=7.3$ MeV; measured $\ensuremath{\sigma}(\ensuremath{\theta})$. Deduced rms radii for picked-up neutrons. Comparisons with Coulomb displacement energies.]

10.1103/physrevc.9.2340

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Citations (10)

Evolution of Unstable Red Giant Envelopes

Symposium - International Astronomical Union (1983)

Y. Tuchman

Two main observable phenomena are directly connected with the dynamical behaviour of Red Giant (R.G.) envelopes: The variability of Mira stars and Planetary Nebulae (P.N.) ejection.

Red giant

Red-giant branch

Asymptotic giant branch

10.1017/s0074180900093773

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Envelope Pulsations of a 1 M_⊙ AGB Star During Thermal Pulses

Symposium - International Astronomical Union (2000)

A. Yaari Y. Tuchman J. Wagenhuber

An abstract is not available for this content so a preview has been provided. As you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Envelope (radar)

Star (game theory)

10.1017/s0074180900003557

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Evolution of Unstable Red Giant Envelopes

Planetary Nebulae (1983)

Y. Tuchman

10.1007/978-94-009-7094-6_29

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Citations (1)

Linear analysis of RV Tauri stars : the resonance hypothesis.

Astronomy and Astrophysics (1993)

Y. Tuchman A. Lèbre M. O. Mennesssier A. Yarri

Models of low mass stars (0.5 M ○ . < M < 0.8 M ○ .) with thin envelopes (< 10 −2 M ○ .) and luminosities between 10 3 L ○ . and 10 4 L ○ ., which probably represent proto planetary nebulae, are found to fit nicely the observed features of RV Tauri variables. The linear nonadiabatic pulsational properties of these models, for an extensive range of initial parameters (masses, luminosities and effective temperatures) are presented. The period of the fundamental mode, in most of these models, turns out to be nearly twice that of the first overtone. This fact raises again (Takeuti & Petersen 1983) the possibility that a simple resonance between the fundamental mode and the first overtone is responsible for the observed, well known, alternating minima in the light curves of RV Tauri stars

Overtone

Variable star

Stellar pulsation

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On the Pulsation Mode of Mira Variables: Nonlinear CalculationsCompared with Radii Observations

The Astrophysical Journal (1999)

A. Yaari Y. Tuchman

Observed radii of Mira variables are compared with theoretical nonlinear calculations. In contrast with previous works, the observed data is found to be compatible with the fundamental nonlinear mode of pulsation.

Mode (computer interface)

Variable star

10.1086/311932

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Citations (21)

A new high /greater than or equal to 6 solar masses/ upper mass limit for planetary nebula formation, and a new high lower mass bound for carbon detonation supernova models

The Astrophysical Journal (1978)

Y. Tuchman N. Sack Z. Barkat

view Abstract Citations (12) References (19) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS A new high (â‰¥ 6 M sun) upper mass limit for planetary nebula formation, and a new high lower mass bound for carbon detonation supernova models. Tuchman, Y. ; Sack, N. ; Barkat, Z. Abstract Envelope ejection leading to a planetary nebula has been recently shown to occur as the terminal point of the Mira stage. The ejection is due to a diverging pulsational instability, not to a dynamical one. It is found that in this case (and for Population I, mixing length = 1 pressure scale height) the upper mass limit for formation of planetary nebulae is at least 6 solar masses. It thus follows that the lower mass limit for realization of carbon detonation model configurations is also at least 6 solar masses. Publication: The Astrophysical Journal Pub Date: November 1978 DOI: 10.1086/182811 Bibcode: 1978ApJ...225L.137T Keywords: Planetary Nebulae; Pulsed Radiation; Stellar Evolution; Stellar Mass; Stellar Models; Supernovae; Carbon; Detonation; Dynamic Stability; Mass Distribution; Astrophysics; Formation:Planetary Nebulae; Planetary Nebulae:Stellar Evolution; Supernovae: Models full text sources ADS |

Stellar mass

10.1086/182811

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Citations (12)

The termination of the asymptotic giant branch phase imposed by helium shell flashes - description and conclusions

Monthly Notices of the Royal Astronomical Society (1984)

Y. Tuchman

The increase in the surface luminosity associated with the well-known helium shell flashes might be a trigger for an early mass ejection process. This phenomenon has a significant influence on the global statistical features of the Mira variables as well as on the mass distribution of white dwarfs. The above situation is analysed by adopting the luminosity behaviour during helium shell flashes presented by Wood & Zarro (1981) to the dynamical picture for the asymptotic giant branch stars given by Tuchman, Sack & Barkat (1979). The main observational implications are described and discussed.

Asymptotic giant branch

10.1093/mnras/208.2.215

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Citations (5)