scholarly journals Variation of the generalized Compton red shift in the Sun

1988 ◽  
Vol 123 ◽  
pp. 447-450
Author(s):  
M. Missana
Keyword(s):  
Solar Spectrum ◽  
Systematic Difference ◽  
Compton Effect ◽  
Point Of View ◽  
Red Shift ◽  
Spectral Lines ◽  
The Sun ◽  
Average Depth ◽  
Made In

The most accurate measurements of red shifts in the solar spectrum, made in different epochs by different astronomers, show a systematic difference, in the average 2 mA° (0.2 pm), that seems quite independent on the wavelengths. Such a result can be explained, at least from a qualitative point of view, by the Compton effect. Indeed a variation of the normalized width U of the spectral lines causes a consequent variation of the Compton red shift: increasing U of the 50%, also the red shift increases of about 0.1 pm. Besides that a variation of the average depth h for the formation of the spectral lines in the reversing layer, may cause, in some model atmospheres a change of the red shift: an increase of about 90 Km for h may induce an increase of about 0.4 pm in the Compton red shift.

The Magnetic Sun from Different Views: A Comparison of the Mean and Background Magnetic Field Observations made in Different Observatories and in Different Spectral Lines

2000 ◽  
Vol 179 ◽  
pp. 209-212
Author(s):  
M. L. Demidov
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Large Scale ◽  
Solar Observatory ◽  
Spectral Lines ◽  
The Sun ◽  
Background Magnetic Field ◽  
The Mean ◽  
Selection Of ◽  
Made In

AbstractA comparison is made of observational data on the mean magnetic field of the Sun from several observatories (a selection of published information and new measurements). Results of correlation and regression analyses of observations of background magnetic fields at the STOP telescope of the Sayan solar observatory in different spectral lines are also presented. Results obtained furnish an opportunity to obtain more unbiased information about large-scale magnetic fields of the Sun and, in particular, about manifestations of strong (kilogauss) magnetic fields in them.

Salyut-4 Observations of Active Regions on the Sun

1977 ◽  
Vol 36 ◽  
pp. 333-367 ◽  
Author(s):  
A.V. Bruns ◽  
G.M. Grechko ◽  
A.A. Gubarev ◽  
P.I. Klimuk ◽  
V.I. Sevastyanov ◽  
...  
Keyword(s):  
Fine Structure ◽  
Spatial Resolution ◽  
Physical State ◽  
High Spatial Resolution ◽  
Solar Spectrum ◽  
Active Regions ◽  
Spectral Lines ◽  
The Sun ◽  
Solar Image ◽  
Solar Plasma

We believe that the examination of the ultraviolet solar spectrum is the most informative tool for the diagnostic of the physical state of the solar plasma. But the well known phenomenon of fine structure of active regions (A.R.), as well as of quiet ones, making spectral lines to be wavy and patchy (across dispersion) demandsa) high spatial resolution on the solar image and b) stigmatic spectra.

Gravitational red shift and time delay of radar echo in f(R)-gravity

2016 ◽  
Vol 13 (04) ◽  
pp. 1650051
Author(s):  
Ying Wang ◽  
Feng He
Keyword(s):  
Time Delay ◽  
Experimental Observation ◽  
Space Time ◽  
Red Shift ◽  
Spectral Lines ◽  
Observation Data ◽  
The Sun ◽  
Schwarzschild Metric ◽  
Radar Echo ◽  
Asymptotic Speed

Sobouti proposes an action-based [Formula: see text] modification of Einstein’s gravity, which admits a similar Schwarzschild metric. A test star moving in such a space–time acquires a constant asymptotic speed at large distances. As we are concerned with two classical tests of Einstein’s theory which are gravitational red shift of spectral lines and time delay of radar echo passing the sun, we shall calculate them in the [Formula: see text]-gravity and show that the results are consistent with the experimental observation data.

IV. Corrections to the computed lengths of waves of light published in the Philosophical Transactions of the year 1868

1872 ◽  
Vol 20 (130-138) ◽  
pp. 21-22
Keyword(s):  
Entire Range ◽  
Solar Spectrum ◽  
Important Change ◽  
Spectral Lines ◽  
Entire Series ◽  
Light Waves ◽  
Actual Measure ◽  
Correction Curve ◽  
Made In ◽  
General Table

The author, after adverting to the process by which in a former paper he had attempted the computation of the Lengths of Waves of Light, for the entire series measured in the Solar Spectrum by Kirchhoff, from a limited number of measured Wave-Lengths, and to the discordances between the results of these computations and the actual measure of numerous wavelengths to which he subsequently had access, calls attention to his remark that means existed for giving accuracy to the whole. The object of the present paper is so to use these means as to produce a table of corrections applicable through the entire range of Kirchhoff’s lines, and actually to apply the corrections to those computed wave-lengths which relate to spectral lines produced by the atmosphere and by many metals. Adopting as foundation the comparisons with Ångström’s and Ditscheiner’s measures given in the former paper, and laying these down graphically, the author remarks that in some parts of the spectrum the agreement of the two experimenters is very close, that in some parts they are irreconcilable, and that in one part (where they agree) there is a peculiarity which leads to the supposition that some important change was made in Kirchhoff’s adjustments. He then explains the considerations on which he has drawn a correction-curve, whose ordinates are to give the corrections applicable to his former computed numbers. A general table of corrections is then given, and this is followed by tables of the Lengths of the Light-Waves for the air and metals as corrected by the quantities deduced from that general table.

scholarly journals Researches in spectrum analysis in connexion with the spectrum of the sun

1878 ◽  
Vol 27 (185-189) ◽  
pp. 279-284
Keyword(s):  
Solar Atmosphere ◽  
Spectrum Analysis ◽  
Solar Spectrum ◽  
Spectral Lines ◽  
The Sun

In a map of the solar spectrum, containing a greatly increased number of lines, such as that upon which I am now engaged, it is possible to seek under favourable conditions the coincidence or non-coincidence of lines due to elements hitherto undetected in the solar atmosphere, on account of their existing in quantities insufficient to give very marked spectral lines. A search has accordingly been made, on the principles laid down in previous communications, for those elements which contain in their spectra long and well-characterised lines in the photographic region.

scholarly journals The Position of the Sun in the HR Diagram

1978 ◽  
Vol 80 ◽  
pp. 89-90
Author(s):  
Don C. Barry
Keyword(s):  
Quantitative Analysis ◽  
Spectral Line ◽  
Spectral Type ◽  
Main Sequence ◽  
Solar Spectrum ◽  
Absolute Magnitude ◽  
Systematic Difference ◽  
The Sun ◽  
The Absolute ◽  
Hr Diagram

Since the absolute magnitude of the Sun is known accurately and the solar spectrumdefinesspectral type G2 V, it would appear that the position of the Sun in the HR diagram is well established. However, the color of the Sun and its metallicity relative to other stars remains controversial. It is known from theory that stellar groups of differing composition will have different main sequences.The observed difference in the strength of the metallic lines in Coma stars relative to Hyades stars is caused by a systematic difference in [Fe/H] of less than 0.2 dex or 50%. Photographs and quantitative measures of the systematic differences between the Hyades and Coma spectra are presented. Visual comparison and quantitative analysis of the solar spectrum relative to Hyades and Coma spectra reveal that the Sun is metal rich similar to the Hyades stars rather than of normal disk metallicity as represented by Coma stars. Evidence is presented showing that the color and spectral line strengths of the Sun are more similar to stars classified G3 and G4 in the literature than G2. If the Hyades modulus is y = 3m.25, the (B-V) color of the Sun must be 0m.65 or redder for the Sun to be on or above the Hyades main sequence.

scholarly journals XVI.—The Temperature of the Fresh-water Lochs of Scotland, with special reference to Loch Ness. With Appendix containing Observations made in Loch Ness by Members of the Scottish Lake Survey

1907 ◽  
Vol 45 (2) ◽  
pp. 407-489 ◽  
Author(s):  
E. M. Wedderburn
Keyword(s):  
Comparative Study ◽  
Special Reference ◽  
Fresh Water ◽  
Cold Water ◽  
Point Of View ◽  
The Sun ◽  
The Subject ◽  
Heating Up ◽  
Indirect Action ◽  
Made In

My object in this paper is not, as the title might suggest, to give a comparative study of the fresh-water lochs of Scotland from the point of view of temperature. I had hoped at one time that this would be possible, and I may again return to this part of the subject of lake temperatures; but the more I have considered the question the more am I convinced that such a comparative study from the observations at my disposal would be based on assumptions too fundamental and too uncertain to make the conclusions reached of any great value. Consider the factors which go to produce variations of temperature as they are given by Professor Forel. Briefly, these are the indirect action of the sun in heating up the atmosphere and the surroundings of the loch, radiation from the loch, the effect of warm or cold water brought into the loch by rivers and by rain.

The Interpretation of Line Profiles

1977 ◽  
Vol 36 ◽  
pp. 191-215
Author(s):  
G.B. Rybicki
Keyword(s):  
Magnetic Fields ◽  
Atomic Physics ◽  
Velocity Fields ◽  
Spectral Lines ◽  
Inhomogeneous Structure ◽  
The Sun ◽  
Line Profiles ◽  
Physical Phenomena

Observations of the shapes and intensities of spectral lines provide a bounty of information about the outer layers of the sun. In order to utilize this information, however, one is faced with a seemingly monumental task. The sun’s chromosphere and corona are extremely complex, and the underlying physical phenomena are far from being understood. Velocity fields, magnetic fields, Inhomogeneous structure, hydromagnetic phenomena – these are some of the complications that must be faced. Other uncertainties involve the atomic physics upon which all of the deductions depend.

BIO-ENERGY FROM PHOTOSYNTHETIC ALLOYS FOR USE IN BIOGUALS AND BIOPRODUCTS

2019 ◽  
pp. 613-618
Author(s):  
Petar Kazakov ◽  
Atanas Iliev ◽  
Emil Ivanov ◽  
Dobri Rusev
Keyword(s):  
Technical Progress ◽  
Point Of View ◽  
Energy Sustainability ◽  
International Activities ◽  
Made In

Significant technical progress has been made in recent years in the development of algae-based bioenergy, and much of industrial and academic R&D projects have diverged from the biofuels strategy. This report summarizes the conclusions of a recently concluded symposium analyzing the prospects for using micro- and macroalgae as a feedstock for biofuels and bioenergy. It discusses international activities for the development of bio-energy and non-energy algae bioproducts, advances in the use of macroalgae (both non-cultivated and cultivated algae). Applications for various biochemical and thermochemical uses, bio-refining capabilities for various products, as well as an in-depth review of the process from the point of view of economy and energy sustainability are also given.

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