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Modisette, J. L.

Publications and source records attributed to Modisette, J. L..

At least 19 records
All sourcesNASA NTRSDOE OSTI
NASA NTRS1982

Mass flow due to heating in a binary system - Application to U Cephei

The possibility of mass flow due to the heating of the cooler component in a close binary system has been investigated. The heating may be caused by irradiation from the hotter companion or by other mechanisms such as the spacial coincidence of non-linear 'g-mode' oscillations in the cooler star. The 2.4-day period binary U Cep, in which gas streaming has been observed, has been chosen for model calculations. Preliminary results show that such a heating of the lower atmosphere of the cooler star could lead to mass flow at an average rate of 10 to the -9th - 10 to the -7th solar mass per year without the star necessarily filling its critical Roche surface.

Kondo, Y.↗
NASA NTRS1980

Mass transfer between binary stars

The transfer of mass from one component of a binary system to another by mass ejection is analyzed through a stellar wind mechanism, using a model which integrates the equations of motion, including the energy equation, with an initial static atmosphere and various temperature fluctuations imposed at the base of the star's corona. The model is applied to several situations and the energy flow is calculated along the line of centers between the two binary components, in the rotating frame of the system, thereby incorporating the centrifugal force. It is shown that relatively small disturbances in the lower chromosphere or photosphere can produce mass loss through a stellar wind mechanism, due to the amplification of the disturbance propagating into the thinner atmosphere. Since there are many possible sources of the disturbance, the model can be used to explain many mass ejection phenomena.

Modisette, J. L.↗
NASA NTRS1979

Balloon-borne ultraviolet stellar spectrograph. I - Instrumentation and observation. II - Highlights of first observational results

A dual star-tracking system and a system including a telescope, an echelle spectrograph, and a SEC vidicon are the chief components of the Balloon-borne Ultraviolet Stellar Spectrograph (BUSS), which has flown four successful missions. The BUSS missions have yielded 81 spectra for 56 stars, recorded with a resolution of 0.1 A in the wavelength range from 2200 to 3400 A. BUSS observations include: profiles of Mg II lines indicating considerable mass flow in early-type supergiants; Mg II features suggesting a cool expanding outer shell above a hotter chromosphere; emission features in Zeta Tau (a shell star) indicating infalling material; and emission features of the Be star Phi Per suggesting mass outflow.

Kondo, Y.↗
NASA NTRS1977

The behavior of the Mg II lines near 2800 A in A, B, and O stars

The equivalent widths of the Mg II resonance doublet and their subordinate lines near 2800 A have been determined in ten stars of spectral types A through O. By combining the current results with previously published results for four F stars, it is found that the total equivalent widths of the Mg II lines follow a pattern and that the maximum in absorption strength occurs in late-A spectral type. Evidence of mass flow has been found in the Algol spectrum together with some other peculiarities. The general behavior of the Mg II lines in stars in this spectral range is also discussed.

Kondo, Y.↗
NASA NTRS1977

Evidence for mass loss in the mid-ultraviolet spectra of Be stars

The spectral region about the Mg II doublet lines near 2800 A of Be and shell stars has been observed. The star Gamma Cas shows narrow components to each resonance doublet line shifted 215 km/s toward shorter wavelengths. The resonance and subordinate lines of Zeta Tau are shifted toward shorter wavelengths by 75 km/s, and the subordinate lines are greatly strengthened. The star Kappa Dra, which is much later in spectral type, shows a comparatively normal doublet spectrum.

Morgan, T. H.↗
NASA NTRS1976

Absolute flux calibration for the Mg II observations near 2800 angstroms

Observations of the Mg II features near 2800 A, obtained with a balloon-borne ultraviolet stellar spectrometer for five stars, have been calibrated against the absolute flux measures from OAO-2 spectrometer results. Equivalent widths of the Mg II resonance doublet and their respective subordinate lines, as well as the emission intensities, were evaluated where applicable.

Kondo, Y.↗
NASA NTRS1976

The behavior of the Mg II doublet features near 2800 A observed in F, A, and B supergiants

The Mg II doublet features near 2800 A were recently observed in F-, A-, and B-type supergiants with a balloon-borne ultraviolet stellar spectrometer. The stars observed are Alpha UMi (F8 Ib), Alpha Per (F5 Ib), Eta Leo (A0 Ib), and Rho Leo (B1 Ib). The Mg II doublet features in Alpha UMi and Alpha Per show emission superposed on photospheric absorption. In the spectrum of Eta Leo, the Mg II lines are in absorption and show shortward-shifted components attributable to mass loss. In the spectrum of Rho Leo, the Mg II lines are primarily a composite of the photospheric and interstellar absorption features. The general behavior of the Mg II lines for supergiants of spectral types M through B are also discussed.

Kondo, Y.↗
NASA NTRS1976

Possible Mg II emission in B stars observed from Copernicus

Four B stars, Alpha Vir, Beta Cen, Alpha Gru, and Beta Lib, were observed with the Copernicus spectrometer at a resolution of 0.1 A in order to investigate the presence of chromospheric emission. Emission was observed in Beta Cen and Alpha Gru, while the results for Alpha Vir and Beta Lib were inconclusive.

Kondo, Y.↗
NASA NTRS1973

The effect of Fe I absorption on the Mg II emission at 2795 A in alpha Orionis

The Fe I absorption line at 2795.01 A is derived from the observations of Mg II resonance emission in alpha Orionis by Kondo et al (1972). A spectrum is synthesized, including Mg II emission and self-absorption and also Fe I absorption, which accounts for the observed asymmetry in the Mg II 2795.5 line and for the discrepancy between the theoretical and observed intensity ratios of the two Mg II lines. The astrophysical significance of this strong Fe I absorption is discussed.

Modisette, J. L.↗
NASA NTRS1972

Observations of the stellar Mg II resonance doublet at 2795 and 2802 A.

Spectrophotometry of the Mg II resonance doublet at 2795.5 and 2802.7 A has been performed for five stars with a balloon-borne telescope and spectrometer. Spectral resolution attained was between 0.25 and 0.5 A. A description of the payload and flight operations is given. In beta Lyr the Mg II doublet displayed P Cygni characteristics, while in gamma Lyr the doublet was observed only in absorption. The star beta Cas shows broad overlapping Mg II absorption lines with possible weak emission at the line bottom. In alpha CMi, both components of the doublet are seen in emission at the bottom of the broad absorption feature. The Mg II doublet in alpha Ori is entirely in emission, with each component showing distinct self-reversal.

Kondo, Y.↗
NASA NTRS1972

Magnetic energy flow in the solar wind.

Discussion of the effect of rotation (tangential flow) of the solar wind on the conclusions of Whang (1971) suggesting an increase in the solar wind velocity due to the conversion of magnetic energy to kinetic energy. It is shown that the effect of the rotation of the sun on the magnetic energy flow results in most of the magnetic energy being transported by magnetic shear stress near the sun.

Modisette, J. L.↗
NASA NTRS1969

Buoyancy and solar spin-down

Rapidly rotating solar interior damping by large scale convection analysis via maximum buoyancy force in water cylinder transition

Modisette, J. L.↗