2 edition of Observations of the Ca II K line in the spectrum of 32 Cygni at the 1965 eclipse found in the catalog.
Observations of the Ca II K line in the spectrum of 32 Cygni at the 1965 eclipse
Kenneth Osborne Wright
by Dept. of Energy, Mines and Resources, Observatories Branch in [Ottawa]
Written in English
|Statement||[by] K. O. Wright and K. H. Hesse.|
|Series||Publications of the Dominion Astrophysical Observatory, Victoria, B.C., v. 13, no. 11, Publications of the Dominion. Astrophysical Observatory ;, v. 13, no. 11.|
|Contributions||Hesse, K. H., joint author.|
|LC Classifications||QB4 .V5 vol. 13, no. 11|
|The Physical Object|
|Number of Pages||322|
|LC Control Number||70528415|
k 1 k 1 k1 A x(t) A cosk t B sink t 2 (4) where: 1 2 /T, is the fundamental frequency (rad/sec) and T is the period, A /2 0 is the amplitude of the zero frequency (D.C.) component, A,B kk are the Fourier coefficients, k 1 is the kth harmonic (integer multiple of the fundamental frequency). The Fourier coefficients A,A,B 0 k k are defined by File Size: KB. The Nature of Solar Prominences Einar Tandberg-Hanssen (auth.) and Kluwer Academic Publishers wanted to pub lish such a book. I, therefore, venture to present this monograph in the hope of kindling the interest of some graduate students in the study of this-probably the most spectacular and often the most beautiful of solar activity.
Spectrum Representation • Extending the investigation of Chapter 2, we now consider signals/waveforms that are composed of multiple sinusoids having different amplitudes, frequencies, and phases () where here is real, is complex, and is the frequency in Hz † We desire a graphical representation of the parameters in () versus frequencyFile Size: KB. BRČEKOVÁ, K. - HANSLMEIER, A, - KUČERA, A. - RYBÁK, J. - WOHL, H. Dynamics of the solar photosphere and chromosphere derived from high-resolution Fe I and Ca II K spectra. - RYBÁK, J. - WOHL, H. High-resolution spectroscopy of a chromosphere subflare: Ca II K line measurement. In Il Nuovo Cimento (IF = ). Vol. 25C, , p.
Full text of "Annals of the Astronomical Observatory of Harvard College" See other formats. 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.
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Observations of the Ca II K line in the spectrum of 32 Cygni at the eclipse / [by] K.O. Wright and K.H. Hesse. QB 4 V5 V NO HN A further study of the triple system H.D. (A.D.S. ) / [by] R.M. Petrie and A.H. Batten. QB 4 V5 V NO HN Observations of the Ca II K line, made within a few months of eclipse, are reviewed for the systems ζ Aurigae, 32 Cygni and 31 Cygni.
The intensities of these lines at a given phase differ from one eclipse to another, and at ingress and at egress for the same by: A set of medium to high-resolution observations of H-alpha and Ca II K lines in a sample of Population I stars is presented in order to examine the systematics of H-alpha absorption profiles and.
Emission in Ca ii (4) in VV Cep. The solid line is the spectrum of VV Cep, SWPobserved March 1 (= ); the dotted line is 31 Cyg as observed during chromospheric eclipse on September 3, SWP Cited by: 5. Using photoelectric observations in the Fe line we obtained line-of-sight velocities at nine different positions on the solar disk, as functions of one horizontal co-ordinate and time.
The exocomet falls towards the star and any absorption line produced by the evaporation of the exocomet is redshifted compared to the absorption line of the star. Observations of HR 10 with the PIONIER (VLTI) and 32 years of radial velocity observations revealed that this exocomet host candidate turned out to be a binary star with each star being surrounded by a circumstellar shell.
This new result can explain. This banner text can have markup. web; books; video; audio; software; images; Toggle navigation. BIBLIOGRAPHY Papers 1. Oke (+ 15 graduate students), A Model for a Helium Star of 1 Solar Mass.
Observations of the He II Line in O– and Of–Stars. Astrophys. J.,-D. Mihalas, Non–LTE E ects on Continuum and Hydrogen–Line Parameters in B– and O– Stars. Astrophys. J., bution. The Ca II K. a) Write down what type of spectrum you see (continuous, emission, absorption).
b) Draw a rough copy of the spectrum you see onto your data table. Show sharp and fuzzy lines, bright and faint lines. c) Color in the spectrum in the appropriate places. You will be shown a mystery gas.
Compare the spectrum of the gas with those on your data Size: KB. 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. Publications of R. Henry (updated May 17 Wednesday).
Gregory Kuri, James M. Overduin, & R. Henry, “Exotic Spacetime Topology as an Alternative to Dark Matter and Energy,” APS April Meeting, M. Akshaya, Jayant Murthy, S. Ravichandran, R. Henry, & James Overduin, Components of the Diffuse Ultraviolet Radiation at High Latitudes, submitted to MNRAS Michael Zemcov.
Title: The spectrum of b2 28 Cygni: Authors: Losh, Hazel Marie: Publication: Publications of the Observatory of the University of Michigan ; v.
4, no. 14, Ann Arbor. The ejection velocities (V ej) were measured from the P Cygni profiles. The measured lines include Hα, Hβ, and Hγ, which have measurable P Cygni profiles from April 16 to June 1 (t = – days); Fe ii recombination lines at, and Å; O i Å; and the Ca ii K line at Å.
Publications of Richard C. Henry R. Henry "The Interstellar Medium," invited paper presented at "Small Missions for Energetic Astrophysics, Ultraviolet to Gamma-Ray," J. Robert Oppenheimer Study Center, Los Alamos Natinal Laboratory, February R. Henry "The Intergalactic Medium," invited paper presented at "Small Missions for Energetic Astrophysics, Ultraviolet to Gamma-Ray.
the four observations independently. Also the Iron line parameters match the values obtained before. The χ2 red yields a value of with dof. As shown in Fig.
2 a deviation between the data points and this pure thermal model is still present in the time averaged spectrum.
Therefore we added a non-thermal component in theFile Size: KB. P Cygni is a LBV (B1 Ia+) which exhibits photometric and spectroscopic this book is about 2 We present observational data from two periods (–82 and –90) pointing to three different variability by: 1.
Answers to spectroscopy questions. Consider the spectrum below. Questions a‐f refer to this spectrum. Is the spectrum above a band spectrum or a line spectrum. This is a band spectra, there are what appear to be two overlapping but wide peaks. (II) had an absorbance of at nm. File Size: KB.
Welcome to the CCSS Integrated Pathway: Mathematics III Student Resource Book. This book will help you learn how to use algebra, geometry, data analysis, and probability to solve problems.
Each lesson builds on what you have already learned. As you participate in classroom activities and use this book, you will master important. spectroscopic observations of the eclipsing binary v cygni: 3; 3: astrophysical journal (2)& tifft wg dh pegasi an rr lyrae star of type c: 1; 2: astrophysical journal (3)& rubin vc radial velocities of distant ob stars in anticenter region of galaxy: 6; 0: Mount Wilson observations of the S indices of selected non-cycling stars suggested their Ca ii H & K emission lay well below that of the contemporary solar minimum (Baliunas and Jastrow, ), from which White et al.
deduced that the K emission from the Sun during the Maunder Minimum may have been as little as 11% that of current cycle by:. The star P Cygni (in the constellation Cygnus, the Swan) is surrounded by an extensive low-density atmosphere. Its spectrum is bright continuous, with many narrow, dark absorption lines and a few bright emission lines.
The bright, continuous part of the spectrum is produced by. Abstract: We have measured the profiles of the Ca II H and K chromospheric emission lines in main sequence stars of spectral type M5-K7 ( solar masses) using multiple high resolution spectra obtained during six years with the HIRES spectrometer on the Keck 1 telescope.
Remarkably, the average FWHM, equivalent widths, and line luminosities of Ca II H and K increase Cited by: The analysis of starlight: Some comments on the development of stellar spectroscopy, – Author links open overlay panel J.B. Hearnshaw. Show more. The principal achievements in stellar spectroscopy from the time of Fraunhofer until are summarised in this article, under the headings spectral classification, stellar radial Cited by: 2.