Gotowe bibliografie tematyczne / Observational astronomy

Gotowa bibliografia na temat „Observational astronomy”

Autor: Grafiati
Data publikacji: 4 czerwca 2021
Data aktualizacji: 27 kwietnia 2022

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Artykuły w czasopismach na temat "Observational astronomy"

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Kim, Yong H. "Teaching Observational Astronomy as a Laboratory Course for Non-Majors". International Astronomical Union Colloquium 105 (1990): 154–58. http://dx.doi.org/10.1017/s0252921100086620.

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Since antiquity, doing astronomy means basically stepping outside, looking upward, and considering the widest environment. Thus any undergraduate astronomy program, no matter how diverse its course offering, is incomplete without observational astronomy. For example, some California community colleges offer several courses including such titles as “Man and the Cosmos,” “Final Stellar States,” “Astronomy Enrichment,” and “Astronomical Myths, Mysteries & Fallacies,” but do not offer “Observational Astronomy.” As a teaching astronomer, I question the wisdom and honesty of such practice of proliferation solely based on sensationalism. An introductory lecture course and an observational lab course must be the core of lower-division undergraduate astronomy education. Anything else, in my opinion, is peripheral.
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Surdin, V. G. "Observational Astronomy: Status 2020". Physics of Atomic Nuclei 83, nr 6 (listopad 2020): 962–64. http://dx.doi.org/10.1134/s1063778820050191.

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TAMURA, Motohide. "New Frontiers of Observational Astronomy". Journal of the Visualization Society of Japan 15, nr 59 (1995): 240–45. http://dx.doi.org/10.3154/jvs.15.59_240.

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Arp, Halton. "Observational Problems in Extragalactic Astronomy". Highlights of Astronomy 9 (1992): 43–62. http://dx.doi.org/10.1017/s153929960000873x.

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AbstractA large number of observations have accumulated which represent baffling mysteries from the standpoint of current astronomy. A sample of the most crucial of these cases is reviewed and updated. Evidence has slowly built up to the point where often each individual object is a formidable challenge to conventional theory. But, most importantly, it is now possible to appreciate the common pattern which mutually reinforces all the separate results.These empirical discordances point directly at known weaknesses in the Big Bane theory of the origin of the universe. New data is used to introduce a proposal which accounts for both the data which gave rise to the Big Bang interpretation and which also satisfies the discordant results which have accumulated over the last quarter of a century. Though perhaps only a primitive beginning, the new interpretation demonstrates that observations need not be discarded because they disagree with current theory. The major conclusion from the cases discussed here is that the present observational paradoxes represent spectacular opportunities to make new and fundamental discoveries about the universe.
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Batten, Alan H. "Observational Astronomy in New Zealand". Journal for the History of Astronomy 46, nr 4 (30.10.2015): 496–97. http://dx.doi.org/10.1177/0021828615593271.

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Zdor, Ye S., i V. S. Chernov. "Space ecology and observational astronomy". Astronomical & Astrophysical Transactions 4, nr 1 (czerwiec 1993): 47–48. http://dx.doi.org/10.1080/10556799308205361.

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CANIZARES, C. R. "High-Tech Astronomy: Observational Astrophysics." Science 244, nr 4906 (19.05.1989): 851. http://dx.doi.org/10.1126/science.244.4906.851.

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Bravo-Alfaro, Hector. "An Undergraduate Program for Astronomy in México". Transactions of the International Astronomical Union 24, nr 3 (2001): 164–65. http://dx.doi.org/10.1017/s0251107x00000614.

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Astronomy in México has an ancient tradition, reinforced during the twentieth century by groups working in theoretical and observational astronomy. During the 1990s, the Great Millimeter Telescope (a single 50-m antenna) has been approved, and a 6-m infrared telescope is under study. Graduate and undergraduate programs must be improved to prepare future Mexican and Latin American astronomers to take advantage of these facilities. To meet the challenge, two traditional Mexican programs (Instituto de Astronomia-UNAM and Instituto Nacional de Astrofisica, Optica y Electronica-INAOE) are updating their graduate programs. Similarly, the Departamento de Astronomía de la Universidad de Guanajuato is joining physicists in the first undergraduate program in México in physics and engineering with an option in astrophysics. This will prepare students for industry, academia or national laboratories, either in physics or astronomy. Jobs in academia have been scarce; many students had to give up their goals after one or two postdoctoral positions. Graduate and undergraduate programs must adjust, by broadening the scope of present programs so that students are better prepared for other job opportunities. We present a B.Sc. program designed by astronomers and physicists to try to address some of these concerns and to prepare the students for either continuing with graduate studies or finding employment in an ever-changing job market. (Co-author is Victor Migenes, Guamajato, México.)
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Govind, Amith, Devarshi Choudhury, Blesson Mathew i Paul K. T. "Astrometry: The Foundation for Observational Astronomy". Mapana - Journal of Sciences 17, nr 1 (1.01.2018): 1–10. http://dx.doi.org/10.12723/mjs.44.1.

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Astronomy has seen unprecedented growth in the past century, due to the rise in multiwavelength observations. The foundation for multiwavelength astronomy is given by Astrometry; the science of position and motion determination of celestial bodies. We present a technique of determining equatorial coordinates of celestial bodies from their pixel coordinates. We also present the subsequent results of using this technique in achieving the initial few steps required for the multiwavelength studies of young open clusters.
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Maffie, James. "Watching the Heavens with a ‘Rooted Heart’: The Mystical Basis of Aztec Astronomy". Culture and Cosmos 12, nr 1 (czerwiec 2008): 31–64. http://dx.doi.org/10.46472/cc.0112.0205.

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Aztec epistemology maintained that humans acquire knowledge of reality mystically using their hearts, not their five senses. What, then, was the epistemological status of observational astronomy? Aztec epistemology assigned a privileged role to mystical knowledge and an ancillary, propaedeutical role to observational astronomy. The epistemological evaluation of observational claims in Aztec astronomy occurred within a context of mystically rooted metaphysical, religious, and astrological background assumptions. These played an essential role in the epistemology of Aztec astronomy.
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Rozprawy doktorskie na temat "Observational astronomy"

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Widicus, Weaver Susanna Leigh Beauchamp Jesse L. "Rotational spectroscopy and observational astronomy of prebiotic molecules /". Diss., Pasadena, Calif. : California Institute of Technology, 2005. http://resolver.caltech.edu/CaltechETD:etd-05162005-153745.

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Corrigan, Ruth T. "Observational manifestations of gravitational lenses". Thesis, University of Cambridge, 1992. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.260611.

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Añez, López José Ignacio. "Observational and theoretical perspective of massive star formation". Doctoral thesis, Universitat de Barcelona, 2021. http://hdl.handle.net/10803/671784.

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In this thesis, we are aimed to better understand the massive star formation process paying special attention to the role of the magnetic field. To do this, we will carry out a multi-scale analysis with a double approach, theoretical and observational. a) The role of the magnetic field in the fragmentation process: the case of G14.225-0.506 In this first work, we study the fragmentation of an infrared dark cloud that has a filamentary structure and two hubs. We will pay special attention to the magnetic field present in the environment of the hubs and we will try to relate it to the different levels of fragmentation that these hubs present. In order to carry out this study, we present the result of the CSO observations at 350 um, towards both hubs, North and South, in the infrared dark cloud G14.225-0.506 (from here G14.2). We also show the analysis of polarization and intensity gradient making use of the method developed by Koch et al. 2012, Koch et al. 2012b. In the N-hub we find a magnetic field with a uniform distribution along the east-west direction. However, in the southern hub the B-field shows a bimodal distribution. The intensity-gradient in the N-hub shows a single local minimum. In the S-hub, the intensity gradient reveals two minima reflecting the bimodal distribution of the magnetic field where each component points to each of the minima of the intensity gradient. Analysis of the maps |delta| and Sigma_B in the N-hub indicates that, in the vicinity of the hub, gravity dominates the magnetic field. We have also estimated the intensity of the magnetic field finding higher values in the N-hub than in the S-hub. This supports the idea that the different levels of fragmentation exhibited by hubs depend on differences in magnetic field. b) Modeling the accretion disk around the high-mass protostar GGD 27-MM1 In this second project, we descend to accretion disk scales to understand how massive stars form and evolve. In this work we have used ALMA observations at a wavelength of 1.14~mm with very high angular resolution that resolve the disk around the massive star GGD27-MM1. Motivated by the similarity of this system to those found in low mass, we have modeled the emission of the disk using the models developed by D'Alessio et al. 2006 for low mass stars. The main objective is to investigate whether the assumptions that are valid for disks around low-mass stars could be extrapolated to the case of massive stars. As a result we have found a very massive disk of about ~5 Msun which represents around 25 % of the stellar mass. This mass is consistent with the calculated dynamic mass. The disk has a radius of ~170 au with a 49º of inclination. We have compared the temperature and density structure obtained with our model with potential functions and show that the GGD~27--MM1 system is a potential template for future similar studies in other high-mass protostars. Specifically, we have found a flared disk with a maximum scale height of ~13 au and a temperature profile that goes from ~150 K on the outside of the disk to ~ 1400 K on the inner edge of the disk. Analysis of the Toomre parameter Q evaluated at the midplane temperature of the disk indicates that the disk is stable up to a radius 100 au. This work shows that D'Alessio's models can be used as a first approximation and also obtain various observational predictions.
En esta tesis, pretendemos contribuir a explicar el proceso de formación de estrellas masivas prestando especial atención al papel del campo magnético. Para ello, realizaremos un análisis multiescala con una doble aproximación, teórica y observacional. Por un lado investigaremos el proceso de acrecimiento a través de un disco de acrecimiento entorno a una estrella de alta masa. a) El papel del campo magnético en el proceso de fragmentación: el caso de G14.225-0.506 En este primer trabajo, estudiamos la fragmentación de una nube oscura infrarroja que presenta una estructura filamentaria y dos hubs. Prestaremos especial atención al campo magnético presente en el entorno de los hubs y trataremos de relacionarlo con los distintos niveles de fragmentación que presentan estos hubs. Para poder llevar a cabo este estudio presentamos el resultado de las observaciones del CSO a 350 masas solares, hacia ambos hubs, Norte y Sur, en la nube oscura infrarroja G14.225-0.506 (desde aquí G14.2). También mostramos el análisis de la polarización y gradiente de intensidad haciendo uso del método desarrollado por (Koch et al. 2012, Koch et al. 2012b). b) El modelado del disco de acrecimiento entorno a la protoestrella masiva GGD 27-MM1 En este segundo proyecto, descendemos hasta escalas de discos de acrecimiento para entender como las estrellas masivas se forman y evolucionan. En este trabajo hemos usado observaciones de ALMA a una longitud de onda de 1.14 mm con muy alta resolución angular (aproximadamente 40 mili-segundos de arco) que resuelven el disco entorno a la estrella masiva GGD27-MM1. El disco se dispone perpendicularmente al espectacular chorro de 10 pc de longitud que emana de la fuente, conocido como HH80-81. Motivados por el parecido de este sistema a los que encontramos en baja masa, hemos modelado la emisión del disco haciendo uso de los modelos desarrollados por D'Alessio et al. 2006 para estrellas de baja masa.
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Kelly, Brandon Charles. "Observational Constraints on the Structure and Evolution of Quasars". Diss., The University of Arizona, 2008. http://hdl.handle.net/10150/193633.

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I use X-ray and optical data to investigate the structure of quasars, and its dependence on luminosity, redshift, black hole mass, and Eddington ratio. In order to facilitate my work, I develop new statistical methods of accounting for measurement error, non-detections, and survey selection functions. The main results of this thesis follow. (1) The statistical uncertainty in the broad line mass estimates can lead to significant artificial broadening of the observed distribution of black hole mass. (2) The z = 0.2 broad line quasar black hole mass function falls off approximately as a power law with slope ~ 2 for M_{BH} > 10^8 M_{Sun}. (3) Radio-quiet quasars become more X-ray quiet as their optical/UV luminosity, black hole mass, or Eddington ratio increase, and more X-ray loud at higher redshift. These correlations imply that quasars emit a larger fraction of their bolometric luminosity through the accretion disk component, as compared to the corona component, as black hole mass and Eddington ratio increase. (4) The X-ray spectral slopes of radio-quiet quasars display a non-monotonic trend with Eddington ratio, where the X-ray continuum softens with increasing Eddington ratio until L / L_{Edd} ~ 0.3, and then begins to harden. This observed non-monotonic trend may be caused by a change in the structure of the disk/corona system at L / L_{Edd} ~ 0.3, possibly due to increased radiation pressure. (5) The characteristic time scales of quasar optical flux variations increase with increasing M_{BH}, and are consistent with disk orbital or thermal time scales. In addition the amplitude of short time scale variability decreases with increasing M_{BH}. I interpret quasar optical light curves as being driven by thermal fluctuations, which in turn are driven by some other underlying stochastic process with characteristic time scale long compared to the disk thermal time scale. The stochastic model I use is able to explain both short and long time scale optical fluctuations.
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Uthas, Helena. "Observational studies of highly evolved cataclysmic variables". Thesis, University of Southampton, 2011. https://eprints.soton.ac.uk/202889/.

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Cataclysmic Variables (CV) are binary systems where a main-sequence star transfers mass onto a white dwarf (WD). According to standard evolutionary theory, angular momentum loss drives CVs to initially evolve from longer to shorter orbital periods until a minimum period is reached (≈ 80 minutes). At roughly this stage, the donors becomes degenerate, expand in size, and the systems move towards longer orbital periods. Theory predicts that 70% of all CVs should have passed their minimum period and have sub-stellar donors, but until recently, no such systems were known. I present one CV showing evidence of harbouring a sub-dwarf donor, SDSS J1507+52. Due to the system’s unusually short orbital period of ≈ 65 minutes, and very high space velocity, two origins for SDSS J1507+52 have been proposed; either the system was formed from a young WD/brown-dwarf binary, or the system is a halo CV. In order to distinguish between these two theories, I present UV spectroscopy and find a metallicity consistent with halo origin. Systems close to the minimum period are expected to be faint and have low accretion rates. Some of these CVs show absorption in their spectra, implying that the underlying WD is exposed. This yields a rare opportunity to study the WD in a CV. I introduce two new systems showing WD signatures in their light curves and spectra, SDSS J1457+51 and BW Sculptoris. Despite the fact that CVs close to the minimum period should be faint, we find systems that aremuch too bright for their orbital periods. Such a system is T Pyxidis – a recurrent nova with an unusually high accretion rate and a photometrically determined period < 2 hours. The systemis ∼ 2 times brighter than any other CV at its period. However, to confirm the status of this unusual star, a more reliable period determination is needed. Here, I present a spectroscopic study of T Pyxidis confirming its evolutionary status as a short-period CV. In this thesis, I discuss what implications these systems may have on the current understanding of CV evolution, and the importance of studying individual systems in general
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Seigar, Marcus S. "Observational studies of the structure of spiral galaxies". Thesis, Liverpool John Moores University, 1998. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.242314.

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Nelson, Andrew Frederick. "Dynamics and observational appearance of circumstellar disks". Diss., The University of Arizona, 1999. http://hdl.handle.net/10150/288969.

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In my thesis I present a study of the dynamics and observational characteristics of massive circumstellar disks in two dimensions (r, φ) using two complimentary hydro-dynamic codes: a 'Smoothed Particle Hydrodynamic' (SPH) code and a 'Piecewise Parabolic Method' (PPM) code. I also study the detection limits available to radial velocity searches for low mass companions to main sequence stars. This thesis is organized as a series of published or submitted papers, connected by introductory and concluding material. I strongly recommend that readers of this abstract obtain the published versions of each of these papers. I first outline the progress which has been made in the modeling of the structure and origins of the solar system, then in chapter 2 (The Astrophysical Journal v502, p342, with W. Benz, F. Adams and D. Arnett), I proceed with numerical simulations of circumstellar disks using both hydrodynamic codes assuming a 'locally isothermal' equation of state. The disks studied range in mass from 0.05M* to 1.0 M* and in initial minimum Toomre Q value from 1.1 to 3.0. Massive disks (M(D) > 0.2 M*) tend to form grand design spiral structure with 1-3 arms, while low mass disks (M(D) ≤ 0.2M*) tend to form filamentary, > 4 armed spiral structures. In chapter 4 (submitted to The Astrophysical Journal with W. Benz and T. Ruzmaikina), I relax the assumption the locally isothermal evolution assumption and instead include simple heating and cooling prescriptions for the system. Under these physical conditions, the spiral arm growth is suppressed in the inner 1/3 of the disks relative to the isothermal evolution and in the remainder, changes character to more diffuse spiral structures. I synthesize spectral energy distributions (SEDs) from the simulations and compare them to fiducial SEDs derived from observed systems. The size distribution of grains in the inner disk can have marked consequences on the near infrared portion of the SED. After being vaporized in a hot midplane region, the grains do not reform quickly into the size distribution on which most opacity calculations are based. In chapter 6 (The Astrophysical Journal v500, p940 with Roger Angel), I examine the limits which may be placed upon the detection of planets, brown dwarfs and low mass stellar companions using radial velocity measurements. I derive an analytic expression describing the amplitude limits for periodic signals which may be obtained from a set of data of known duration, number of measurements and precision. In chapter 7, I outline several problems which may be profitably addressed by building on this work. (Abstract shortened by UMI.)
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Stempels, Henricus Cornelis. "An Observational Study of Accretion Processes in T Tauri Stars". Doctoral thesis, Uppsala : Acta Universitatis Upsaliensis : Univ.-bibl. [distributör], 2003. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-3420.

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Endicott, Thomas G. "Effect of Observational Cadence on Orbit Determination for Synthetic Near-Earth Objects". Thesis, University of Massachusetts Boston, 2017. http://pqdtopen.proquest.com/#viewpdf?dispub=10617372.

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Near-Earth Objects (NEOs) are generally small, dark, and fast-moving. Multiple observations over time are necessary to constrain NEO orbits. Orbits based on observational data are inherently uncertain. Here we describe code written in Python and Fortran used to generate synthetic asteroids and compare calculated orbital fit based on noisy ephemeris using the a distance criteria, D-value. Observational sessions separated by more than one month produce very good orbital fits (low D-values) even at the highest noise level. Daily observational sessions show the highest D-values, as expected, since observed points on the orbital ellipse are not well separated. D-value is closely correlated to differences in the eccentricity and inclination of compared orbits.

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Moffat, Anthony F. J. "Observational overview of clumping in hot stellar winds". Universität Potsdam, 2007. http://opus.kobv.de/ubp/volltexte/2008/1763/.

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In the old days (pre ∼1990) hot stellar winds were assumed to be smooth, which made life fairly easy and bothered no one. Then after suspicious behaviour had been revealed, e.g. stochastic temporal variability in broadband polarimetry of single hot stars, it took the emerging CCD technology developed in the preceding decades (∼1970-80’s) to reveal that these winds were far from smooth. It was mainly high-S/N, time-dependent spectroscopy of strong optical recombination emission lines in WR, and also a few OB and other stars with strong hot winds, that indicated all hot stellar winds likely to be pervaded by thousands of multiscale (compressible supersonic turbulent?) structures, whose driver is probably some kind of radiative instability. Quantitative estimates of clumping-independent mass-loss rates came from various fronts, mainly dependent directly on density (e.g. electron-scattering wings of emission lines, UV spectroscopy of weak resonance lines, and binary-star properties including orbital-period changes, electron-scattering, and X-ray fluxes from colliding winds) rather than the more common, easier-to-obtain but clumping-dependent density-squared diagnostics (e.g. free-free emission in the IR/radio and recombination lines, of which the favourite has always been Hα). Many big questions still remain, such as: What do the clumps really look like? Do clumping properties change as one recedes from the mother star? Is clumping universal? Does the relative clumping correction depend on $dot{M}$ itself?
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Książki na temat "Observational astronomy"

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Birney, D. Scott. Observational astronomy. Cambridge: Cambridge University Press, 1991.

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Birney, D. Scott. Observational astronomy. Cambridge [England]: Cambridge University Press, 1991.

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Sarma, K. V. Observational astronomy in India. Kerala: Dept. of Sanskrit, University of Calicut, 1990.

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Observational astronomy: Techniques and instrumentation. Cambridge: Cambridge University Press, 2011.

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Observational astrophysics. Wyd. 3. Heidelberg: Springer, 2012.

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Léna, Pierre. Observational astrophysics. Wyd. 2. Berlin: Springer, 1998.

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Observational astrophysics. Berlin: Springer-Verlag, 1988.

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Dark energy: Observational and theoretical approaches. Cambridge, UK: Cambridge University Press, 2010.

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Chromey, Frederick R. To measure the sky: An introduction to observational astronomy. Cambridge: Cambridge University Press, 2010.

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To measure the sky: An introduction to observational astronomy. Cambridge: Cambridge University Press, 2010.

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Części książek na temat "Observational astronomy"

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Longair, Malcolm S. "Radio Astronomy and Cosmology". W Observational Cosmology, 3–10. Dordrecht: Springer Netherlands, 1998. http://dx.doi.org/10.1007/978-94-011-5238-9_1.

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Rohlfs, K., i T. L. Wilson. "Observational Methods". W Astronomy and Astrophysics Library, 166–91. Berlin, Heidelberg: Springer Berlin Heidelberg, 1996. http://dx.doi.org/10.1007/978-3-662-03266-4_7.

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Wilson, Thomas L., i Susanne Hüttemeister. "Observational Methods". W Astronomy and Astrophysics Library, 39–44. Berlin, Heidelberg: Springer Berlin Heidelberg, 2000. http://dx.doi.org/10.1007/978-3-642-57001-8_8.

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Branch, David, i J. Craig Wheeler. "Observational Properties". W Astronomy and Astrophysics Library, 483–517. Berlin, Heidelberg: Springer Berlin Heidelberg, 2017. http://dx.doi.org/10.1007/978-3-662-55054-0_20.

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Fridman, Alexei M., i Nikolai N. Gorkavyi. "Observational Data". W Astronomy and Astrophysics Library, 21–57. Berlin, Heidelberg: Springer Berlin Heidelberg, 1999. http://dx.doi.org/10.1007/978-3-662-03918-2_2.

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Rohlfs, K., i T. L. Wilson. "Observational Methods". W Astronomy and Astrophysics Library, 166–91. Berlin, Heidelberg: Springer Berlin Heidelberg, 2004. http://dx.doi.org/10.1007/978-3-662-05394-2_7.

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Maccacaro, Tommaso, Suzanne Romaine i Jurgen H. M. M. Schmitt. "Logn-Logs Slope Determination in Imaging X-ray Astronomy". W Observational Cosmology, 597–99. Dordrecht: Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-3853-3_62.

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Arp, Halton. "Observational Problems in Extragalactic Astronomy". W Highlights of Astronomy, 43–62. Dordrecht: Springer Netherlands, 1992. http://dx.doi.org/10.1007/978-94-011-2828-5_3.

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Steele, John M. "Babylonian Observational and Predictive Astronomy". W Handbook of Archaeoastronomy and Ethnoastronomy, 1855–62. New York, NY: Springer New York, 2014. http://dx.doi.org/10.1007/978-1-4614-6141-8_191.

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Aerts, C., J. Christensen-Dalsgaard i D. W. Kurtz. "Observational Techniques for Asteroseismology". W Astronomy and Astrophysics Library, 295–335. Dordrecht: Springer Netherlands, 2009. http://dx.doi.org/10.1007/978-1-4020-5803-5_4.

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Streszczenia konferencji na temat "Observational astronomy"

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Cline, David. "OBSERVATIONAL NEUTRINO ASTRONOMY". W Workshop on Extra Solar Neutrino Astronomy. WORLD SCIENTIFIC, 1988. http://dx.doi.org/10.1142/9789814541411.

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Primack, Joel R. "Observational Gamma-ray Cosmology". W HIGH ENERGY GAMMA-RAY ASTRONOMY: 2nd International Symposium on High Energy Gamma-Ray Astronomy. AIP, 2005. http://dx.doi.org/10.1063/1.1878394.

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Halzen, Francis. "High-Energy Neutrino Astronomy". W THE NEW COSMOLOGY: Conference on Strings and Cosmology; The Mitchell Symposium on Observational Cosmology. AIP, 2004. http://dx.doi.org/10.1063/1.1848331.

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Lee, Joong Y., Donald Figer, Elizabeth Corrales, Jonathan Getty i Lynn Mears. "HgCdTe detectors grown on silicon substrates for observational astronomy". W High Energy, Optical, and Infrared Detectors for Astronomy VIII, redaktorzy Andrew D. Holland i James Beletic. SPIE, 2018. http://dx.doi.org/10.1117/12.2313401.

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Kaifu, Norio. "Rapid Progress and Limitation of Observational Astronomy in Japan". W Accelerating the Rate of Astronomical Discovery. Trieste, Italy: Sissa Medialab, 2010. http://dx.doi.org/10.22323/1.099.0003.

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Cramer, Claire E., Steven W. Brown, Keith R. Lykke, John T. Woodward, Stephen Bailey, David J. Schlegel, Adam S. Bolton i in. "Tunable laser techniques for improving the precision of observational astronomy". W SPIE Astronomical Telescopes + Instrumentation, redaktorzy Ramón Navarro, Colin R. Cunningham i Eric Prieto. SPIE, 2012. http://dx.doi.org/10.1117/12.925198.

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Baryshev, Yu V., i S. A. Oschepkov. "Gravitation theory in multimessenger astronomy II: crucial observational tests based on GW and optical observations". W SN 1987A, Quark Phase Transition in Compact Objects and Multimessenger Astronomy. Институт ядерных исследования Российской академии наук, 2018. http://dx.doi.org/10.26119/sao.2020.1.52285.

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van der Klis, M. "Kilohertz quasi-periodic oscillations-observational overview". W X-RAY ASTRONOMY: Stellar Endpoints,AGN, and the Diffuse X-ray Background. AIP, 2001. http://dx.doi.org/10.1063/1.1434653.

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Marchis, Franck, Paul G. Kalas, Marshall D. Perrin, Quinn M. Konopacky, Dmitry Savransky, Bruce Macintosh, Christian Marois i James R. Graham. "Large collaboration in observational astronomy: the Gemini Planet Imager exoplanet survey case". W SPIE Astronomical Telescopes + Instrumentation, redaktorzy Alison B. Peck, Robert L. Seaman i Chris R. Benn. SPIE, 2016. http://dx.doi.org/10.1117/12.2233313.

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Perivolaropoulos, L. "Accelerating Universe: Observational Status and Theoretical Implications". W RECENT ADVANCES IN ASTRONOMY AND ASTROPHYSICS: 7th International Conference of the Hellenic Astronomical Society. AIP, 2006. http://dx.doi.org/10.1063/1.2348048.

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Raporty organizacyjne na temat "Observational astronomy"

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Kleinmann, Susan G. Observational Study and Analysis of Point Sources Found by the Infrared Astronomy Satellite. Fort Belvoir, VA: Defense Technical Information Center, kwiecień 1991. http://dx.doi.org/10.21236/ada248416.

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Helfand, David J. A Program of Ground-Based Astronomy to Complement Einstein Observations. Fort Belvoir, VA: Defense Technical Information Center, grudzień 1986. http://dx.doi.org/10.21236/ada179331.

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Zilberman, Mark. Methods to Test the “Dimming Effect” Produced by a Decrease in the Number of Photons Received from Receding Light Sources. Intellectual Archive, listopad 2020. http://dx.doi.org/10.32370/iaj.2437.

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Streszczenie:
The hypothetical “Dimming Effect” describes the change of the number of photons arriving from a moving light source per unit of time. In non-relativistic systems, the “Dimming effect” may occur due to the growing distance of light sources moving away from the receiver. This means that due to the growing distance, the photons continuously require more time to reach the receiver, which reduces the number of received photons per time unit compared to the number of emitted photons. Understandably, the proposed “Dimming effect” must be tested (confirmed or rejected) through observations. a. This article provides the formula for the calculation of “Dimming effect” values using the redshift parameter Z widely used in astronomy. b. The “Dimming effect” can possibly be detected utilizing the orbital movement of the Earth around the Sun. In accordance to the “Dimming effect”, observers on Earth will view 1.0001 more photons per time unit emitted by stars located near the ecliptic plane in the direction of the Earth orbiting the Sun. And, in contrast, observers will view only 0.9999 photons per time unit emitted by stars located near the ecliptic plane in the direction opposite to the Earth orbiting the Sun. Calculating precise measurements of the same stars within a 6-month period can possibly detect this difference. These changes in brightness are not only for specific stars, as the change in brightness takes place for all stars near the ecliptic in the direction of the Earth’s orbit around the Sun and in the opposite direction. c. The “Dimming effect” can possibly be detected in a physics laboratory using a moving light source (or mirror) and photon counters located in the direction of travel and in the opposite direction. d. In theory, Dilation of time can also be used for testing the existence of the “Dimming effect.” However, in experiments on Earth this effect appears in only the 14th digit after the decimal point and testing does not appear to be feasible. e. Why is it important to test the “Dimming effect?” If confirmed, it would allow astronomers to adjust values of "Standard Candles" used in astronomy. Since “Standard Candles” are critical in various cosmological models, the “Dimming effect” can correct models and/or reveal and support new models. If it is proved that the “Dimming effect” does not exist, it will mean that the number of photons arriving per unit of time does not depend on the speed of the light source and observer, which is not so apparent.
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