The solution of the homogeneous plane problem of the motion of a piston in an ideal heat-conducting gas

Volosevich, P. P.; Kurdyumov, S. P.; Busurina, L.N.; Krus, V.P.

doi:10.1016/0041-5553(63)90131-9

Cited by 11 publications

(4 citation statements)

References 2 publications

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“…The sum is taken over all levels for which the threshold photoionization frequency ν j ≤ β k T /h; then hν ≥ β k T . 7 Katsova et al [5] and Livshits et al [6] give the following physical parameters of the source of quasi-blackbody radiation at wavelengths around 4500 Å: ∆z ≈ 10 km, N H ≈ 2•10 15 cm −3 , T ≈ 9000 K ∼ 0.8 eV. It is easy to see that the corresponding single-temperature (T ai = T e ) homogeneous plane layer cannot generate the small Balmer jump (the bottom curve of Fig.…”

Section: Introduction Grinin and Sobolevmentioning

confidence: 96%

“…( 5) of the present article, respectively. From this table, 7 It is evident that the exponent "39" in Eq. ( 4) of study [1] should read "-39;" and the temperature T should be raised to a power of "-1/2."…”

Section: Introduction Grinin and Sobolevmentioning

confidence: 97%

“…In solving a single-temperature 3 system of gas dynamics equations "with the given boundary and initial conditions and the calculated loss and heating functions" [5], they found that two disturbances "propagate downward and upward" [5] "from the formed zone of high pressure" [6]. The disturbance propagating toward the photosphere ("downward" [5]) "is described in subsequent times by a solution of the type of the second-kind temperature wave [7]." "The latter is characterized by a subsonic-velocity propagation of the thermal wave [temperature jump]" [6], "in front of which a [non-stationary] shock wave ..." develops [5].…”

Section: Introduction Grinin and Sobolevmentioning

confidence: 99%

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Origin of the Blue Continuum Radiation in the Flare Spectra of dMe Stars

Morchenko

2016

Astrophysics

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Calculations of the emission spectrum of a homogeneous plane layer of pure hydrogen plasma taking into account nonlinear effects (the influence of bremsstrahlung and recombination radiation of the layer itself on its Menzel factors) [9] show that the blue component of the optical continuum during the impulsive phase of large flares on dMe stars originates from the near-photospheric layers [1]. The gas behind the front of a stationary radiative shock wave propagating in the red dwarf chromosphere toward the photosphere is not capable of generating the blackbody radiation observed at the maximum brightness of the flares.

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Section: Introduction Grinin and Sobolevmentioning

confidence: 96%

Section: Introduction Grinin and Sobolevmentioning

confidence: 97%

Section: Introduction Grinin and Sobolevmentioning

confidence: 99%

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Origin of the Blue Continuum Radiation in the Flare Spectra of dMe Stars

Morchenko

2016

Astrophysics

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“…According to this model, the blue component of the optical continuum is formed in a chromospheric condensation. The condensation is located between a temperature jump and the front of a downward shock wave (the second-kind temperature wave [5]). The physical parameters of this source of white-light continuum (N H ≈ 2 • 10 15 cm −3 , T ≈ 9000 K, and thickness ∆z ≈ 10 km) lie in the range of the layer parameters in the model by Grinin and Sobolev [1] (N H ∼ 10 15 − 10 17 cm −3 , T ∼ 5000 − 20000 K, and ∆z 10 km).…”

Section: Introductionmentioning

confidence: 99%

Continuum and line emission of flares on red dwarf stars

Morchenko

Bychkov²,

Livshits³

2015

Astrophys Space Sci

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The emission spectrum has been calculated of a homogeneous pure hydrogen layer, which parameters are typical for a flare on a red dwarf. The ionization and excitation states were determined by the solution of steady-state equations taking into account the continuum and all discrete hydrogen levels. We consider the following elementary processes: electron-impact transitions, spontaneous and induced radiative transitions, and ionization by the bremsstrahlung and recombination radiation of the layer itself. The BibermanHolstein approximation was used to calculate the scattering of line radiation. Asymptotic formulae for the escape probability are obtained for a symmetric line profile taking into account the Stark and Doppler effects. The approximation for the core of the H−α line by a gaussian curve has been substantiated.The spectral intensity of the continuous spectrum, the intensity of the lines of the Balmer series and the magnitude of the Balmer jump have been calculated. The conditions have been determined for which the Balmer jump and the emission line intensities above the continuum decrease to such low values that the emission spectrum can be assumed to be continuum as well as the conditions at which the emission spectrum becomes close to the blackbody.

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Initial phase of developing dynamic perturbations in a nonlinearly heat conducting gas

Romanov¹,

Stytsyna²

1989

J Appl Mech Tech Phys

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The solution of the homogeneous plane problem of the motion of a piston in an ideal heat-conducting gas

Cited by 11 publications

References 2 publications

Origin of the Blue Continuum Radiation in the Flare Spectra of dMe Stars

Origin of the Blue Continuum Radiation in the Flare Spectra of dMe Stars

Continuum and line emission of flares on red dwarf stars

Initial phase of developing dynamic perturbations in a nonlinearly heat conducting gas

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