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Karp, A. H.

Publications and source records attributed to Karp, A. H..

10 records
All sourcesNASA NTRSDOE OSTI
NASA NTRS1979

Deep photospheric flows in Tau Scorpii

From analysis of weak, unblended, ultraviolet lines observed in Tau Scorpii by Copernicus, the same line widths and the same slightly blue-depressed wings as found in the upper photospheric lines of the visual region are found. In addition, a radial-velocity discrepancy of about 6 km/s between weak and strong lines in the 1000-1300-A region is found. These results are in quantitative agreement with one another and with the results of the visual region. They imply that a flow of material is present even in the deep photosphere of this star. However, one cannot yet specify the geometry of the flow (outward-radial versus temperature-weighted convection columns). At the least, this flow alters the expected radiation-driven flow solution close to the photosphere. At the most, it could provide the heating of a chromosphere or a corona just outside the photosphere, as required by the imperfect flow model.

Smith, M. A.↗
NASA NTRS1975

Hydrodynamic models of a Cepheid atmosphere. III - Line spectrum and radius determinations

Line profiles are computed on the basis of the moving atmospheres from the hydrodynamic models investigated by Karp (1975). It is found that the velocity gradients in the atmosphere can be used to explain the apparent, slightly supersonic microturbulence. The total observed microturbulence is seen to be consistent with the linear sum of the classical microturbulence and that caused by the velocity gradients.

Karp, A. H.↗
NASA NTRS1975

A modified Henyey method for computing radiative transfer hydrodynamics

The implicit hydrodynamic code of Kutter and Sparks (1972), which is limited to optically thick regions and employs the diffusion approximation for radiative transfer, is modified to include radiative transfer effects in the optically thin regions of a model star. A modified Henyey method is used to include the solution of the radiative transfer equation in this implicit code, and the convergence properties of this method are proven. A comparison is made between two hydrodynamic models of a classical Cepheid with a 12-day period, one of which was computed with the diffusion approximation and the other with the modified Henyey method. It is found that the two models produce nearly identical light and velocity curves, but differ in the fact that the former never has temperature inversions in the atmosphere while the latter does when sufficiently strong shocks are present.

Karp, A. H.↗
NASA NTRS1975

Hydrodynamic models of a Cepheid atmosphere. I - Deep envelope models

The implicit hydrodynamic code of Kutter and Sparks has been modified to include radiative transfer effects. This modified code has been used to compute deep envelope models of a classical Cepheid with a period of 12 days. It is shown that in this particular model the hydrogen ionization region plays only a small role in producing the observed phase lag between the light and velocity curves. The cause of the bumps on the model's light curve is examined, and a mechanism is presented to explain those Cepheids with two secondary features on their light curves. This mechanism is shown to be consistent with the Hertzsprung sequence only if the evolutionary mass-luminosity law is used.

Karp, A. H.↗
NASA NTRS1975

Hydrodynamic models of a Cepheid atmosphere

Instead of computing a large number of coarsely zoned hydrodynamic models covering the entire atmospheric instability strip, the author computed a single model as well as computer limitations allow. The implicit hydrodynamic code of Kutter and Sparks was modified to include radiative transfer effects in optically thin zones.

Karp, A. H.↗
NASA NTRS1974

Hydrodynamic models of a cepheid atmosphere

A method for including the solution of the transfer equation in a standard Henyey type hydrodynamic code was developed. This modified Henyey method was used in an implicit hydrodynamic code to compute deep envelope models of a classical Cepheid with a period of 12(d) including radiative transfer effects in the optically thin zones. It was found that the velocity gradients in the atmosphere are not responsible for the large microturbulent velocities observed in Cepheids but may be responsible for the occurrence of supersonic microturbulence. It was found that the splitting of the cores of the strong lines is due to shock induced temperature inversions in the line forming region. The adopted light, color, and velocity curves were used to study three methods frequently used to determine the mean radii of Cepheids. It is concluded that an accuracy of 10% is possible only if high quality observations are used.

Karp, A. H.↗
NASA NTRS1973

Velocity gradients and microturbulence in Cepheids.

Variations of the microturbulent velocity with phase and height in the atmosphere have been reported in classical Cepheids. It is shown that these effects can be understood in terms of variations of the velocity gradient in the atmospheres of these stars.

Karp, A. H.↗
NASA NTRS1972

Velocity gradients and microturbulence in Cepheids

Variations of the microturbulent velocity with phase and height in the atmosphere were reported in classical Cepheids. It is shown that these effects can be understood in terms of variations of the velocity gradient in the atmospheres of these stars.

Karp, A. H.↗
NASA NTRS1972

A modification of the Avrett-Krook temperature-correction procedure.

In the course of developing a computer program for blanketed model stellar atmospheres, it was found that near the surface the Avrett-Krook temperature correction procedure (1963) has poor convergence properties. The problem is most apparent when frequencies shortward of the Lyman discontinuity are included. Slightly different assumptions have been made to improve the convergence.

Karp, A. H.↗