The line response function of stellar atmospheres and the effective depth of line formation     

Jacques M. Beckers  Robert W. Milkey 《Solar physics》1975,43(2):289-292

The response function defines the response of line profiles to a depth variation of such atmospheric parameters as velocity, magnetic field and turbulence. The properties of this function are derived and compared with the so-called contribution function.Operated by the Association of Universities for Research in Astronomy, Inc., under contract with the National Science Foundation.  相似文献   

Addendum to paper on Roter Kamm     

Robert S. Dietz 《Meteoritics & planetary science》1966,3(1):33-34

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Pressure and temperature dependence of the elastic properties of polycrystalline trevorite (NiFe₂O₄)     

Robert C. Liebermann 《Physics of the Earth and Planetary Interiors》1972,6(5):360-365

Ultrasonic pulse-superposition measurements at 298 K as a function of hydrostatic pressure to 3 kb for polycrystalline trevorite (NiFe₂O₄; 1.0% porosity) yield values of the isotropic elastic properties as shown in the table to the right.  相似文献   

Electromagnetic Induction in a Thin Strip     

Robert L. Parker 《Geophysical Journal International》1967,14(1-4):487-495

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The History of the International Seismological Summary     

Robert Stoneley 《Geophysical Journal International》1970,20(4):343-349

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Chromospheric heating above supergranular boundaries     

Robert W. Milkey 《Solar physics》1970,14(1):62-76

A geometrical optics technique developed in order to study energy transport by weak fast-mode hydromagnetic shock waves in a non-homogeneous, anisotropic medium has been applied to the problem of the heating of the chromosphere in the regions of intensified magnetic field which occur above the boundaries of supergranular cells. The results of the calculation indicate that there should be a temperature enhancement in the regions of the chromospheric network. This temperature enhancement is advanced as a possible mechanism for the origin of the observed calcium emission network.Publications of the Goethe Link Observatory, Indiana University, No. 106.Presently at Los Alamos Scientific Laboratories, Los Alamos, New Mexico.  相似文献   

Polar magnetic fields of the Sun: 1960–1971     

Robert Howard 《Solar physics》1972,25(1):5-13

Observations of the magnetic fields in the polar regions of the Sun are presented for the period 1960–1971. At the start of this interval the fields at the two poles were consistently of opposite sign and averaged around 1 G. Early in 1961 the field in the south decreased suddenly and the field in the north decreased in strength slowly over the next few years. By the mid-1960's the fields at both poles were quite weak and irregular. Throughout the period of these observations the fields at both poles often showed a remarkable tendency to vary in unison. About the middle of 1971 the north polar field became significantly positive, first at lower latitudes, then above 70 °. An autocorrelation analysis of the polar fields in the north shows a weak rotation peak, indicating significant features in these regions. A comparison of field strengths in the east and west quadrants in the north suggests that even at the extreme polar latitudes the following polarity fields are inclined slightly toward the rotation and the preceding polarity field lines are inclined slightly to trail the rotation.  相似文献   

A large-scale pattern in the solar magnetic field     

John M. Wilcox  Robert Howard 《Solar physics》1968,5(4):564-574

A clearly evident large-scale pattern in the interplanetary magnetic field during 1964 is used to search for a similar large-scale pattern in the solar magnetic field. It is found that such a pattern did exist in the photospheric field observations on both sides of the equator over a range of at least 40°N to 35°S. The pattern is basically similar at all these latitudes, and differs from that to be expected from solar differential rotation in three important respects. It is found that the solar magnetic pattern changed at all latitudes investigated within an interval of a few solar rotations.  相似文献   

The Systematic Error in Seismic Location     

Robert Underwood  Roy C. Lilwall 《Geophysical Journal International》1969,17(5):521-526

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Energy losses of low-energy photoelectrons to thermal electrons     

Robert W. Schunk  Paul B. Hays 《Planetary and Space Science》1971

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