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  • 1
    Online Resource
    Online Resource
    Editor’s Preface
    Cambridge University Press (CUP) ; 1979
    In:  International Astronomical Union Colloquium Vol. 53 ( 1979-08), p. v-v
    Details
    In: International Astronomical Union Colloquium, Cambridge University Press (CUP), Vol. 53 ( 1979-08), p. v-v
    Type of Medium: Online Resource
    ISSN: 0252-9211
    URL: Article
    DOI: 10.1017/S0252921100075618
    Language: English
    Publisher: Cambridge University Press (CUP)
    Publication Date: 1979
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  • 2
    Online Resource
    Online Resource
    Effects of Superfluidity on Spheroidal Oscillations of Neutron Stars
    Cambridge University Press (CUP) ; 1994
    In:  International Astronomical Union Colloquium Vol. 147 ( 1994), p. 586-590
    Details
    In: International Astronomical Union Colloquium, Cambridge University Press (CUP), Vol. 147 ( 1994), p. 586-590
    Abstract: In the limit of short wavelengths, it has been shown that superfluidity significantly affects wave propagation in neutron stars. Here we abandon the short-wavelength restriction and extend these calculations to global oscillation modes. In the present analysis, the solid crust of the neutron star is divided into an outer crust and an inner crust, and a superfluid of neutrons coexists with the solid lattice in the inner crust. We have computed several low-order global spheroidal modes for l = 2 both with and without superfluidity. We find that superfluidity in the inner crust affects the frequency spectra of acoustic ( p -) modes, shear ( s -) modes, and interfacial ( i -) modes, although the surface gravity ( g -) modes are not affected at all.
    Type of Medium: Online Resource
    ISSN: 0252-9211
    URL: Article
    DOI: 10.1017/S0252921100026658
    Language: English
    Publisher: Cambridge University Press (CUP)
    Publication Date: 1994
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  • 3
    Online Resource
    Online Resource
    Some Properties of Hot, High-Gravity, Pure Helium Atmospheres
    Cambridge University Press (CUP) ; 1979
    In:  International Astronomical Union Colloquium Vol. 53 ( 1979-08), p. 125-129
    Details
    In: International Astronomical Union Colloquium, Cambridge University Press (CUP), Vol. 53 ( 1979-08), p. 125-129
    Abstract: Model atmosphere analyses of white dwarf spectra have contributed significantly to our understanding of the properties of degenerate stars.: In particular, the pioneering investigations of Bues (1970), Strittmatter and Wickramasinghe (1971) and Shipman (1972) have provided the first reliable determinations of the effective temperature and surface gravity of these objects (see Shipman 1979 and Weidemann 1978 for recent results). We now know with certainty that the hydrogen-rich white dwarf sequence extends at least over the range T e ∽ 6000 – 60.000K. In contrast, the hottest identified helium-rich white dwarfs seem to reach T e ~ 25.000K only, a puzzling result since the progenitors of DB white dwarfs should presumably also be helium-rich.
    Type of Medium: Online Resource
    ISSN: 0252-9211
    URL: Article
    DOI: 10.1017/S0252921100075813
    Language: English
    Publisher: Cambridge University Press (CUP)
    Publication Date: 1979
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  • 4
    Online Resource
    Online Resource
    Crystallization of a classical, one-component coulomb plasma
    Elsevier BV ; 1969
    In:  Physics Letters A Vol. 28, No. 10 ( 1969-2), p. 706-707
    Details
    In: Physics Letters A, Elsevier BV, Vol. 28, No. 10 ( 1969-2), p. 706-707
    Type of Medium: Online Resource
    ISSN: 0375-9601
    URL: Article
    DOI: 10.1016/0375-9601(69)90699-9
    RVK:
    UA 1000 ; UA 6580.A
    Language: English
    Publisher: Elsevier BV
    Publication Date: 1969
    detail.hit.zdb_id: 1466603-0
    detail.hit.zdb_id: 208865-4
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  • 5
    Online Resource
    Online Resource
    Non-Radial Oscillations of Degenerate Dwarfs: A Theoretical Review
    Cambridge University Press (CUP) ; 1976
    In:  International Astronomical Union Colloquium Vol. 29 ( 1976), p. 259-285
    Details
    In: International Astronomical Union Colloquium, Cambridge University Press (CUP), Vol. 29 ( 1976), p. 259-285
    Abstract: The current status of the theory of non-radial oscillations of white dwarfs and hydrogen shel1-burning degenerate stars, in the linear, quasi-adiabatic approximation, is reviewed. Relevant aspects of the thermal structure of such stars are summarized, and several problem areas requiring further investigation are identified. Among the most interesting and important of these are the question of the existence of g modes in white dwarfs; the nature of the excitation mechanisms for non-radial oscillations; the possibility of tidal excitation; the problem of mode-coupling between pulsations and convection; and the question of the effects of a solid, crystallizing core.
    Type of Medium: Online Resource
    ISSN: 0252-9211
    URL: Article
    DOI: 10.1017/S025292110006200X
    Language: English
    Publisher: Cambridge University Press (CUP)
    Publication Date: 1976
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  • 6
    Online Resource
    Online Resource
    A Possible Identification of the Quasi-Periodic Oscillations in Dwarf Novae
    Cambridge University Press (CUP) ; 1979
    In:  International Astronomical Union Colloquium Vol. 53 ( 1979-08), p. 509-509
    Details
    In: International Astronomical Union Colloquium, Cambridge University Press (CUP), Vol. 53 ( 1979-08), p. 509-509
    Abstract: Quasi-periodic oscillations on timescales from ~30 sec to 150s have been observed in several dwarf novae during outburst. These oscillations have been qualitatively interpreted as pulsations of the accretion disks in these systems. We explore this suggestion quantitatively by examining the non-radial pulsation properties of viscous accretion disks in the linear, quasi-adiabatic approximation. The weak coupling of the pulsation modes in the radial direction is consistent with the interpretation of these modes as arising in individual disk annuli with periods and eigenfunctions characteristic of the properties of the annulus. The periods of the oscillations, which are periodic in ϕ, z, and t, are shown to be directly proportional to the Keplerian period of the annulus. The existence of a luminosity maximum at some radial position in the disk suggests that the annuli near this position will be the dominant contributors to the observed oscillations. For parameters typical of dwarf novae, the corresponding oscillation periods are ~ 20s, with a range from ~10s to ~ 150s. We suggest that these modes correspond to the observed quasi-periodic oscillations.
    Type of Medium: Online Resource
    ISSN: 0252-9211
    URL: Article
    DOI: 10.1017/S0252921100076594
    Language: English
    Publisher: Cambridge University Press (CUP)
    Publication Date: 1979
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  • 7
    Online Resource
    Online Resource
    Magnetic Field Decay in the Non-superfluid Regions of Neutron Star Cores
    Cambridge University Press (CUP) ; 1994
    In:  International Astronomical Union Colloquium Vol. 147 ( 1994), p. 591-595
    Details
    In: International Astronomical Union Colloquium, Cambridge University Press (CUP), Vol. 147 ( 1994), p. 591-595
    Abstract: We consider a simple model for the evolution of a poloidal magnetic field initally trapped in a region containing normal npe matter within the outerliquid core of a neutron star. We have performed numerical computations for neutron stars with masses of 1.4, 1.6, and 1.7 M ⊙ that undergo very rapid cooling due to the direct Urca process. Because the timescale for the magnetic field decay is directly proportional to T 2 , such a cooling history produces a rapid decline in the magnetic-field strength B , even for B as low as ∼ 10 12 G. In particular, we show that an initially quasi-homogeneous magnetic field of strength B = 10 12 G declines during the first ∼ 1 Myr.
    Type of Medium: Online Resource
    ISSN: 0252-9211
    URL: Article
    DOI: 10.1017/S025292110002666X
    Language: English
    Publisher: Cambridge University Press (CUP)
    Publication Date: 1994
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  • 8
    Online Resource
    Online Resource
    On Radiative Transfer Near the Plasma Frequency at Strong Coupling
    Cambridge University Press (CUP) ; 1994
    In:  International Astronomical Union Colloquium Vol. 147 ( 1994), p. 581-585
    Details
    In: International Astronomical Union Colloquium, Cambridge University Press (CUP), Vol. 147 ( 1994), p. 581-585
    Abstract: The effects of strong coupling on the frequency-averaged optical characteristics of plasmas, such as the Rosseland mean-free-path, are considered. The general expression for the Rosseland mean opacity has been analyzed in terms of the transverse dielectric function of a dense plasma and the frequency-dependent effective collision frequency. The corresponding values of the absorption coefficient and the refractive index for a dense plasma are presented at ω ≤ ω p up in obvious forms.
    Type of Medium: Online Resource
    ISSN: 0252-9211
    URL: Article
    DOI: 10.1017/S0252921100026646
    Language: English
    Publisher: Cambridge University Press (CUP)
    Publication Date: 1994
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  • 9
    Online Resource
    Online Resource
    Production of Planetary Nebulae
    Cambridge University Press (CUP) ; 1968
    In:  Symposium - International Astronomical Union Vol. 34 ( 1968), p. 400-406
    Details
    In: Symposium - International Astronomical Union, Cambridge University Press (CUP), Vol. 34 ( 1968), p. 400-406
    Abstract: For various reasons, we have been studying evolution in the pre-white dwarf phase at Rochester. Our attention to the relevance of this work to planetary nebulae came as a result of calculations of the evolution of a one solar-mass iron star carried out at Rochester by S. Vila. Here the neutrino processes drive the peak luminosity to log L / L ⊙ =4·26, at an effective temperature log T eff =5·53. Although these models are brighter than 100 L ⊙ for 500 000 years, they are brighter than 1000 L ⊙ for 4000 years, and exceed 10000 L ⊙ for 900 years. We are therefore near the luminosity of the planetary-nebula nuclei, but considerably hotter, for a period of the order of the planetary lifetimes. Except for the temperature discrepancy, these models are in rough agreement with the observationally determined evolutionary sequence found by O'Dell (1963) and by Harman and Seaton (1964) and Seaton (1966).
    Type of Medium: Online Resource
    ISSN: 0074-1809
    URL: Article
    DOI: 10.1017/S0074180900020921
    Language: English
    Publisher: Cambridge University Press (CUP)
    Publication Date: 1968
    SSG: 16,12
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  • 10
    Online Resource
    Online Resource
    Implications of White-Dwarf Crystallization for the Chemical Composition of the Planetary Nuclei
    Cambridge University Press (CUP) ; 1968
    In:  Symposium - International Astronomical Union Vol. 34 ( 1968), p. 425-427
    Details
    In: Symposium - International Astronomical Union, Cambridge University Press (CUP), Vol. 34 ( 1968), p. 425-427
    Abstract: It now seems to be reasonably well-established that the central stars of planetary nebulae evolve directly into white dwarfs. Evidently a knowledge of the chemical composition of the white dwarfs would therefore be of considerable importance in helping to identify the point in the evolution at which the mechanism responsible for expulsion of the nebular shell becomes operative. For this reason I would like to present some evidence which provides a direct suggestion for the internal composition of some of the white dwarfs and to examine briefly the implications of this suggestion for the relation between the planetary nuclei and the white dwarfs.
    Type of Medium: Online Resource
    ISSN: 0074-1809
    URL: Article
    DOI: 10.1017/S0074180900020970
    Language: English
    Publisher: Cambridge University Press (CUP)
    Publication Date: 1968
    SSG: 16,12
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