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2 edition of Chromospheric K-Lite of ch 2 in the Spectrum of 31 Cygni. found in the catalog.

Chromospheric K-Lite of ch 2 in the Spectrum of 31 Cygni.

Canada. Dept. of Energy, Mines and Resources. Observatories Branch.

Chromospheric K-Lite of ch 2 in the Spectrum of 31 Cygni.

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Published .
Written in English


Edition Notes

1

SeriesCanada Dominion Astrophysical Observatory Pub -- V.11,no.02
ContributionsMckellar, A., Aller, L.H., Odgers, G.J.
ID Numbers
Open LibraryOL21904457M

Ni ± ± ± Notes. Values are normalized to Si≡ Only the statistical uncertain-ties are given. The absolute intensity (with combined statistical and sys-tematic uncertainties) for silicon at MeV nucleon−1 is ( ± ) ×. The two methods were: a) the Barnes-Evans relation for (B-V), and 2) d 2 /R 2, with distances, d, from Hipparcos (for 5 of the 6 stars), and stellar radii, R, from the Stefan-Boltzmann relation (where temperature is known from spectral classification of KPNO coude feed spectra of the six stars by colleague F.C. Fekel (COE, TN St. U.), and. Hardy, F.R.S., ; Chemistry Programme at the British Association Meeting at Portsmouth, £; 2 6-dibenzoyl-2 6-dimethylheptane and aa'-tetramethylpimelic Acid, A. Haller, E. Bauer, the Decomposition of Water by Metals, M. Kern baum, the Catalytic Preparation of Fatty Esters in the Wet Way, J. B. Senderens, J. Aboulenc, ; Osmotic. Recent research on the solar-stellar system has been triggered by a host of recent observational data, in particular from space based observations. For this conference the major topics selected centered on new measurement capabilities (magnetic fields and infrared, with specific emphasis on the new.


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Chromospheric K-Lite of ch 2 in the Spectrum of 31 Cygni. by Canada. Dept. of Energy, Mines and Resources. Observatories Branch. Download PDF EPUB FB2

Summary. Chromospheric activity, as seen by the presence of a central K 2 emission in the Ca ii K λ nm line, is studied in F- and G-stars of all luminosity classes. K 2 equivalent widths have been measured and corresponding absolute K 2 fluxes (power per unit area at the stellar surface) calculated.

Large K 2 equivalent widths and thus easily detectable chromospheres occur only for Cited by: 1. The spectacular changes of CH Cyg spectrum during the last period of activity and the flickering in short wavelength light suggest the possibility of rapid line variations (Walker et al.,).

In November a series of spectral observations has been accomplished at Rozhen Observatory to investigate the : T. Tomov, D. Raikova. HIGH-LEVEL CHROMOSPHERIC Chromospheric K-Lite of ch 2 in the Spectrum of 31 Cygni. book AND THEIR BEHAVIOUR IN SUN-SPOT SPECTRA.

FOWLER] on *FREE* shipping on qualifying : A. FOWLER. The Spectrum of CH Cygni in is a composite of emission components and the underlying M-type giant spectrum.

In order to obtain an accurate emission line profile, the latter needs to be removed. As for a spectral standard, the spectrogram of HD(RZ Arietis, M6 III) was obtained with the use of the same spectrograph on Octo Cited by: 5. It is found that the mass Chromospheric K-Lite of ch 2 in the Spectrum of 31 Cygni.

book, 1 / 2, is less than 15 for the two systems, Aurigae and 31 Cygni, where the data are well determined, and masses of approximately 8 for the giant K star and 6. Ahmad I.A. () A “flash spectrum” of cool absorption in 31 CYGNI: A direct observation of the reversing layer?.

In: Linsky J.L., Stencel R.E. (eds) Cool Stars, Stellar Systems, and the Sun. Lecture Notes in Physics, vol Author: Imad A.

Ahmad. The Å emission index computed from basal profiles shows a significantly reduced modulation (as compared with one derived from the observed profiles) corresponding to the Sun's rotation. For basal contribution of the Ca II K line, the peak in power spectrum corresponding to Chromospheric K-Lite of ch 2 in the Spectrum of 31 Cygni.

book rotation is. The measurements suggest there is a peak in main sequence chromospheric activity near B - V =which corresponds approximately to spectral type FO. We confirm the presence of stellar Lya emission in the spectrum of the A7 V star αAg1, but find no emission in the spectra of 10 other late A-type by: Abstract We present new 14 high-resolution echelle spectra to discuss the level of chromospheric activity of DM UMa in {He I} D 3, {Na I} D 1, D 2, Hα, and {Ca II} infrared triplet lines (IRT).It is the first time to discover the emissions above the continuum in the {He I} D 3 lines on February 9 and The emission on February 9 is the strongest one Chromospheric K-Lite of ch 2 in the Spectrum of 31 Cygni.

book detected for DM UMa. The fluxes in passbands nm wide and centered on the Ca II H and K emission cores have been monitored in stars of spectral type F2-M2 on or near the main sequence in a continuation of an.

This banner text can have markup. web; books; video; audio; software; images; Toggle navigation. Boro Saikia, C. Marvin et al.: Chromospheric activity catalogue of cool stars. B-V l o g plot. There is a concentration of inactive stars close to the solar. The planet-star interaction is manifested in many ways.

It was found out that a close-in exoplanet causes small but measurable variability in the cores of a few lines in the spectra of several stars which corresponds to the orbital period of the exoplanet. Stars with and without exoplanets may have different properties.

The main goal of our study is to search for influence which exoplanets Cited by: Analysis of high-resolution IR spectra of CH Cygni shows that the star is a triple system with a short period orbit of just over 2 yrs. The period ratio of seven for CH Cyg is the smallest known.

the spectrum, that are sensitive to luminosity and other parameters. The Ca II triplet lines at, are ideal candidates for studying their sensitivity to var-ious stellar parameters in cool stars.

These lines are due to transitions between the upper 4p 2P 1=2;3=2 levels and the lower metastable 3d 2D 3=2;5=2 levels. The same upperCited by: Chromospheric Structure Derived from Flash Spectra of the Total Solar Eclipse 3 final n(h)is obtained from equation (2).

According to the study by Zirker (), the emission gradient of the metallic lines is equal to the total hydrogen density gradient. If in equation (1) n is replaced with the to. C.I. Short & J.G. Doyle: Chromospheric line blanketing and the hydrogen spectrum in M dwarfs to derive chromospheric diagnostics by comparing the relative response of the various series of the Hi spectrum (Lyman to rium and line formation physics in chromospheric models.

Computational method Atmospheric models. VV Cephei (M2 Iab + B0–2 V) is the only known ζ Aur binary that has an M-type supergiant. Studies of its atmospheric eclipses provide a valuable extension to what can be learned by eclipse mapping, but are fraught with many challenges.

The space-UV absorption spectrum is extremely rich, and line blending is : Philip D. Bennett, Wendy Hagen Bauer.

According toLeitherer (), for ˙ M ≈ 10 −6 M yr −1, R = 5 R and v(r = R), τ (Hα) is a few × for a temperature of the underlying photosphere of 10 4 K (we note, however, that.

The age-metallicity relation of the solar neighbourhood is studied using a sample of late-type dwarfs. This sample was built from the intersection of photometric catalogues with chromospheric activity surveys of the Mount Wilson group.

For these stars, metallicities were estimated from uvby data, and ages were calculated from their chromospheric emission levels using a new metallicity Author: H. Rocha-Pinto, W. Maciel, John Scalo, Chris Flynn.

Abstract: We perform X-ray studies of the shell-type supernova remnant (SNR) gamma-Cygni associated with the brightest EGRET unidentified source 3EG J+ In addition to the thermal emissions with characteristic temperature of kT = keV, we found an extremely hard X-ray component from several clumps localized in the northern part of the by: The second variable star to be described was the eclipsing variable Algol, by Geminiano Montanari in ; John Goodricke gave the correct explanation of its variability in Chi Cygni was identified in by G.

Kirch, then R Hydrae in by G. Maraldi. By ten variable stars were known. The formation of low-mass (M ★ ≲ 2 M ⊙) stars in molecular clouds involves accretion disks and jets, which are of broad astrophysical interest.

Accreting stars represent the closest examples of these phenomena. Star and planet formation are also intimately connected, setting the starting point for planetary systems like our own.

The ultraviolet (UV) spectral range is particularly Author: P. Christian Schneider, H. Moritz Günther. Methods. To analyse the chromospheric activity of stars, we exploited our own** and publicly available archival spectra***, measured the equivalent widths of the cores of Ca II H and K lines, and used them to trace their activity.

Subsequently, we searched for their dependence on the orbital parameters and the mass of the exoplanet. by: chapter model binary balmer shown spectra observed profiles temperature accretion disk observations winds equation optical spectrum wind density shell ray region phase line stars envelopes envelope shock formation.

Comparing chromosphere and photosphere. Whilst the photosphere has an absorption line spectrum, the chromosphere's spectrum is dominated by emission particular, one of its strongest lines is the H α at a wavelength of nm; this line is emitted by a hydrogen atom whenever its electron makes a transition from the n=3 to the n=2 energy level.A wavelength of nm is in the red.

The derived masses of M 1 = M solar, M 2 = M solar for the giant and dwarf, respectively, constrain the choice of models for fitting evolutionary tracks in the (logT eff, logL) plane. The giant is almost certainly on its first ascent of the red giant branch. You can write a book review and share your experiences.

Other readers will always be interested in your opinion of the books you've read. Whether you've loved the book or not, if you give your honest and detailed thoughts then people will find new books that are right for them.

Free ebooks since ASCA View of the Supernova Remnant Gamma Cygni (G+): Bremsstrahlung X-ray Spectrum from Loss-flattened Electron Distribution Item Preview remove-circle Share or Embed This Item. For given spectrum of the electron population, the ratio of the bremsstrahlung X- and gamma-ray fluxes depends on the position of the ``Coulomb break'' in.

A series of dark spectral lines among the colors of the continuous spectrum. Kirchoff's 3rd Law A cool, transparent gas in front of a source of a continuous spectrum that produces an absorption line spectrum.

We obtained Hubble STIS spectra of three nova-like variables: V Cygni, V Oph, and - the only confirmed nova-like variable known to be below the period. The star P Cygni (in the constellation Cygnus, the Swan) is surrounded by an extensive low-density atmosphere.

Its spectrum consists of a bright, continuous spectrum with many narrow, dark absorption lines and few bright emission lines. The Dark absorption lines are produced by: By what factor is the amount of light gathered by the m diameter Kreck telescope on Mauna Kea, Hawaii, greater.

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