Увійти

Готові списки джерел за темами / Double stars

Добірка наукової літератури з теми "Double stars"

Автор: Grafiati

Опубліковано: 4 червня 2021

Оновлено: 3 березня 2023

Оформте джерело за APA, MLA, Chicago, Harvard та іншими стилями

Оберіть тип джерела:

Ознайомтеся зі списками актуальних статей, книг, дисертацій, тез та інших наукових джерел на тему "Double stars".

Біля кожної праці в переліку літератури доступна кнопка «Додати до бібліографії». Скористайтеся нею – і ми автоматично оформимо бібліографічне посилання на обрану працю в потрібному вам стилі цитування: APA, MLA, «Гарвард», «Чикаго», «Ванкувер» тощо.

Також ви можете завантажити повний текст наукової публікації у форматі «.pdf» та прочитати онлайн анотацію до роботи, якщо відповідні параметри наявні в метаданих.

Зміст

Статті в журналах
Дисертації
Книги
Частини книг
Тези доповідей конференцій
Звіти організацій

Статті в журналах з теми "Double stars":

1

Vilkki, E. U. "New Double Stars." Publications of the Astronomical Society of the Pacific 100 (December 1988): 1540. http://dx.doi.org/10.1086/132361.

Повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

2

Xin-Lian, Luo, Bai Hua, and Zhao Lei. "Double Degenerate Stars." Chinese Physics Letters 25, no. 7 (July 2008): 2378–81. http://dx.doi.org/10.1088/0256-307x/25/7/013.

Повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

3

Urban, S. E., T. E. Corbin, G. L. Wycoff, and B. D. Mason. "Problems of Using Hipparcos Astrometry of Double Stars." International Astronomical Union Colloquium 180 (March 2000): 97–103. http://dx.doi.org/10.1017/s0252921100000178.

Повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

Анотація:

AbstractThe current optical realization of the International Celestial Reference System is the Hipparcos main catalog in its entirety. This paper demonstrates that a subset of the main catalog stars — specifically those marked as double (“C” stars), acceleration solution (“G”), variability induced movers (“V”), and stochastic solution stars (“X”) — is of much lower quality than the majority of the catalog. Stars marked as suspected doubles (“S”) were investigated and found to show few problems. The authors have put forth a resolution (Resolution 2, this conference) to remove the C, G, V, and X stars, in addition to the Hipparcos orbit stars (“O stars”), from the optical realization of the reference frame.

4

Agati, Jean-Louis, Sébastien Caille, André Debackère, Pierre Durand, Florent Losse, René Manté, Florence Mauroy, et al. "Activities and Achievements of the Double Star Committee of the Société Astronomique de France." Proceedings of the International Astronomical Union 2, S240 (August 2006): 509–26. http://dx.doi.org/10.1017/s174392130700645x.

Повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

Анотація:

In a synthesis article (see ref. below), the double star expert Paul COUTEAU put the work of French pioneers of double stars observation in the perspective of the double star work carried in the world. After Antoine Yvon VILLARCEAU and Camille FLAMMARION, one prominent pioneer of double stars was Robert JONCKHEERE (1888–1974), an amateur before circumstances prompted him to become a professional astronomer, who devoted his life to double stars. Kenneth Glyn Jones wrote a biography and Charles Fehrenbach his obituary. Jean-Claude Thorel studied his life and career in double star observations (see Section 10 below). In the 1930s, another precursor of the Commission des Étoiles Doubles, Maurice DURUY (1894–1984) invented the micrometer with a comparison star, and applied the diffraction micrometer invented by Ejnar Hertzsprung to the measure of double stars, which he regularly observed at Nancy with a 275-mm telescope, at Lyon with a 162-mm telescope and in his observatory of Beaume-Mêle with a 40-cm and later a 60-cm telescope at Le Rouret (Alpes–Maritimes). He measured standard pairs of the list of Paul Muller and published his measures in the Journal des Observateurs; these measures requested by Paul Muller aimed at comparisons of between observers. He also collaborated with the Webb Society of Great Britain; Glyn Jones published his astronomical biography. Already in 1924, the pediatrician Paul BAIZE (1901–1995) had started the measurement of double stars as an amateur. He was granted permission to measure them with the 38-cm of the Paris Observatory and made an impressive number of measures during his long “career" (24044). He also made orbit calculations and established a formula for the calculation of dynamic parallaxes in 1946. He wrote articles explaining new observation techniques devoted to double stars in the magazine L'Astronomie and continued his astronomical activity until the beginning of the 1990s. Glyn Jones published an astronomical biography of Paul Baize. In the 1960s, Bernard CLOUET and the late Robert SAGOT (1910–2006) made double star observations for the book which was then in preparation under the title La revue des constellations. Their measures remained unpublished; but publication of the measures made by Robert SAGOT is in preparation. At about the same time, the neurology professor Jacques LE BEAU (1908–1998) made the acquaintance of renowned professional astronomer Paul COUTEAU and learned from him how to measure double stars. Each year, he stayed for two weeks at Nice and conducted his observations with the 50-cm refractor of the Nice Observatory. In 1978, Paul COUTEAU published the first book in French devoted to double stars: L'observation des étoiles doubles visuelles. That book triggered the interest of more amateur astronomers for double stars and indirectly influenced the creation of a group of double star observers which was transformed into the Commission des Étoiles Doubles

5

Novakovic, B., and N. Todorovic. "Orbits of four double stars." Serbian Astronomical Journal, no. 172 (2006): 21–25. http://dx.doi.org/10.2298/saj0672021n.

Повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

Анотація:

We present orbits of four double stars. Orbits of stars WDS 23516+4205 = ADS 17050 and WDS 18239+5848 = ADS 11336 were calculated for the first time. Orbits of double stars WDS 02022+3643 = ADS 1613 and WDS 18443+3940 = ADS 11635 were revised. We have also determined their masses, dynamical parallaxes and ephemerides.

6

Rezaei, Zeinab. "Double dark matter admixed neutron star." International Journal of Modern Physics D 27, no. 16 (December 2018): 1950002. http://dx.doi.org/10.1142/s0218271819500020.

Повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

Анотація:

The dark matter (DM) in neutron stars can exist from the lifetime of the progenitor or when captured by this compact object. The properties of DM that enter the neutron stars through each step could be different from each other. Here, we investigate the structure of neutron stars which are influenced by the DM in two processes. Applying a generalization of two-fluid formalism to three-fluid one and the equation-of-state from the rotational curves of galaxies, we explore the structure of double DM admixed neutron stars. The behavior of the neutron and DM portions for these stars is considered. In addition, the influence of the DM equations of state on the stars with different contributions of visible and DM are studied. The gravitational redshift of these stars in different cases of DM equations of state is investigated.

7

Zinnecker, H., C. Scarfe, C. Allen, T. Armstrong, W. Hartkopf, R. D. Mathieu, A. Tokovinin, and M. Valtonen. "Commission 26: Double and Multiple Stars (Etoiles Doubles Et Multiples)." Transactions of the International Astronomical Union 24, no. 1 (2000): 186–89. http://dx.doi.org/10.1017/s0251107x00002856.

Повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

Анотація:

This triennial report (1996-1999) reviews the subject from a somewhat personal angle, mostly related to binary star formation and young binary star populations – a subject whose time had come in the early 1990s and is now in full swing.Many astronomers have searched for binary systems among main-sequence stars, and two large-scale surveys published in 1991 and 1992 have already become classics. Well before they became famous for finding extrasolar planets (see below), observing teams led by Michel Mayor (Geneva Observatory) and Geoffrey Marcy (San Francisco State Univ., now Univ. of Calif, at Berkeley) spent many years searching for low-mass stellar companions of nearby stars. The late Antoine Duquennoy and Mayor surveyed all solar-type dwarfs (spectral types F7 through G9) within 20 pc of the Sun, while Debra Fischer and Marcy studied stars with somewhat lower mass (M dwarfs) slightly nearer to the Sun.

8

Isobe, Syuzo, and Mikinori Ni-Ino. "Formation rate of triple stars relative to double stars." Astrophysics and Space Science 224, no. 1-2 (February 1995): 491–92. http://dx.doi.org/10.1007/bf00667920.

Повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

9

Zulevic, D. J., G. M. Popovic, and R. Pavlovic. "Micrometer measurements of double stars." Serbian Astronomical Journal, no. 161 (2000): 25–31. http://dx.doi.org/10.2298/saj0061025z.

Повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

Анотація:

A set of 71 measurements of double and multiple stars, carried out with the Large Zeiss Refractor 65/1055 cm of the Belgrade Observatory, is communicated. The bulk of these measurements, 41 in all, unpublished yet, is due to late D. Zulevic.

10

Worley, Charles E., and Brian D. Mason. "Micrometer Measures of Double Stars." Astronomical Journal 116, no. 2 (August 1998): 917–30. http://dx.doi.org/10.1086/300475.

Повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

Більше джерел

Дисертації з теми "Double stars":

1

Bascoul, Guillaume Pierre. "Double-diffusive convection in stars." Thesis, University of Cambridge, 2007. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.613006.

Повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

2

Komonjinda, Siramas. "A study of binary star orbits using precise radial velocity measurements with the HERCULES spectrograph." Thesis, University of Canterbury. Department of Physics and Astronomy, 2008. http://hdl.handle.net/10092/1590.

Повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

Анотація:

Orbits of spectroscopic binary systems have been studied for more than a century. Over three thousand orbits of spectroscopic binary systems have been derived. These orbits are based on the radial velocities measured from the spectra recorded by a photographic plate to a high precision spectrum observed from a modern spectrograph. In many cases, the shape of the orbit was assumed to be circular, of hence the eccentricity is zero. This assumption is based on the fact that a small eccentricity (e < 0.1) measured from the observed data might be a result from the error of observations or from the intrinsic variation of a spectroscopic binary system. Sixteen southern spectroscopic binary systems, including twelve single-lined binaries and four double-lined binaries, were selected to study in this research program. These systems were assumed to have circular orbits or have very nearly circular orbits (e < 0.1) from their previous published solutions. The HERCULES spectrograph was used in conjunction with the 1-m McLellan telescope at Mt John University Observatory to collect the spectra of these systems. The observations, taken from October 2004 to August 2007, comprised about 2000 high-resolution spectra of spectroscopic binary systems and standard radial-velocity stars. Radial velocities of spectroscopic binary systems were measured from these spectra and orbital solutions of the systems were derived from these radial velocities. It was found that from HERCULES data, we are able to achieve high-precision orbital solutions of all the systems studied. The best-fit solutions can be improved as much as 70 times from the literature’s orbital solutions. It has been found that the precision of a system depends on the rotational velocities of the components as well as the level of their chromospheric activity. We are able to confirm the eccentricity in the orbit of only one of the selected spectroscopic binary systems, HD194215. Its eccentricity is 0.123 29 ± 0.000 78. The small eccentricities of other systems are not confirmed. There are four systems; HD22905, HD38099, HD85622 and HD197649, that have circular orbital solutions from the large errors in their measured eccentricities. Two systems, HD77258 and HD124425, have too small eccentricities, e = 0.000 85±0.000 19 and 0.002 60 ± 0.000 99 to be acceptable. An intrinsic variation is a presumed cause of the spurious eccentricities derived from the data of the other eight systems. Photometric data from Mt John University Observatory service photometry program, as well as the photometric data from the Hipparcos satellite and information of these systems from the literature, using various methods and instruments, give a wider view on the systems’ behaviour. It is possible that the spurious eccentricities derived for these systems result from the eclipsing behaviour of a system (HD50337), or from the nature of the components, such as, the distortion of their shape (HD352 and HD136905), their chromospheric activity (HD9053, HD3405, HD77137, HD101379 and HD155555), or stellar pulsation (HD30021). Models of the active chromosphere system, HD101379, have been simulated. An analysis of synthetic radial velocity data shows that spots on the star’s photosphere can cause a spurious eccentricity. The values of the spurious eccentricity and the longitude of periastron are dependent on the spot size, the spot temperature, and the position of the spots.

3

Bauer, Christina, of Western Sydney Nepean University, and Faculty of Science and Technology. "Astrometric observations of wide southern double stars." THESIS_FST_XXX_Bauer_C.xml, 1995. http://handle.uws.edu.au:8081/1959.7/251.

Повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

Анотація:

Observations were made of 309 binary systems between RA 17h - 07h and Dec -70 degrees to -60 degrees. The images were calibrated against pairs measured for CCD astometry. Measurements were made of separations, position angles and differential magnitudes. Uncertainties in position angle and separation were 7.8o/p and 0.16 arcseconds respectively. The position angles, separations and differential V magnitudes were compared with WDS figures. It was determined that only 29% _+ 5% of the observed pairs had undergone significant movement since the last previous measurement, which agrees with the results of a survey of the WDS. A statistical study of 1q77 pairs found that the spread of calculated separations agreed with those found by other authors, while the distribution of periods, while falling within the range(s) calculated by other authors, were significantly longer. A short-arc fitting program was tested using data derived from the published orbit of Centauri before being applied to seven observed pairs. Orbits could be calculated for six of the seven pairs. For four of these pairs the observed movement may be due to proper motion rather than orbital motion
Master of Science (Hons)

4

Bauer, Christina. "Astrometric observations of wide southern double stars." Thesis, View thesis, 1995. http://handle.uws.edu.au:8081/1959.7/251.

Повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

Анотація:

Observations were made of 309 binary systems between RA 17h - 07h and Dec -70 degrees to -60 degrees. The images were calibrated against pairs measured for CCD astometry. Measurements were made of separations, position angles and differential magnitudes. Uncertainties in position angle and separation were 7.8o/p and 0.16 arcseconds respectively. The position angles, separations and differential V magnitudes were compared with WDS figures. It was determined that only 29% _+ 5% of the observed pairs had undergone significant movement since the last previous measurement, which agrees with the results of a survey of the WDS. A statistical study of 1q77 pairs found that the spread of calculated separations agreed with those found by other authors, while the distribution of periods, while falling within the range(s) calculated by other authors, were significantly longer. A short-arc fitting program was tested using data derived from the published orbit of Centauri before being applied to seven observed pairs. Orbits could be calculated for six of the seven pairs. For four of these pairs the observed movement may be due to proper motion rather than orbital motion

5

Bauer, Christina. "Astrometric observations of wide southern double stars /." View thesis, 1995. http://library.uws.edu.au/adt-NUWS/public/adt-NUWS20030827.113613/index.html.

Повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

6

Wainwright, C. L. "The effects of spin-orbit coupling on gravitational wave uncertainties." Pomona College, 2007. http://ccdl.libraries.claremont.edu/u?/stc,20.

Повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

Анотація:

Paper discusses the expected uncertainty of orbital parameters of binary stars as measured by the space-based gravitational wave observatory LISA (Laser Interferometer Space Antenna) and how the inclusion of spin in the model of the binary stars affects the uncertainty. The uncertainties are found by calculating the received gravitational wave from a binary pair and then performing a linear least-squares parameter estimation. The case of a 1500 solar mass black hole that is 20 years from coalescing with a 1000 solar mass black hole--both of which are 50 x 10^6 light years away--is analyzed, and the results show that the inclusion of spin has a negligible effect upon the angular resolution of LISA but can increase the accuracy in mass and distance measurements by factors of 15 and 65, respectively.

7

Chanamé, Domínguez Julio César. "Topics of galactic structure and stellar and chemical evolution." Connect to resource, 2005. http://rave.ohiolink.edu/etdc/view?acc%5Fnum=osu1126128106.

Повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

Анотація:

Thesis (Ph. D.)--Ohio State University, 2005.
Title from first page of PDF file. Document formatted into pages; contains xv, 286 p.; also includes graphics (some col.). Includes bibliographical references (p. 275-286). Available online via OhioLINK's ETD Center

8

Xu, Huangjian. "A study of the binary radio star LSI +61 303." Thesis, University of British Columbia, 1987. http://hdl.handle.net/2429/28358.

Повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

Анотація:

We present new 6 cm observations of the binary radio, X-ray and ɿ -ray star GT0236+610 (LSI+61°303) obtained in August 1984 and September 1986. Ve calculate an improved period for the source's periodic radio outbursts of 26.50 ± 0.03 days. No significant period derivative was found. Based on an analysis of 201 flux density measurements from 1977 August to 1986 September, we find evidence for a possible 4 year modulation of the amplitude of the 26.50 day periodic radio outbursts. A precessing jet model for this long period modulation is discussed.
Science, Faculty of
Physics and Astronomy, Department of
Graduate

9

Rainger, Paul P. "Studies of low-mass interacting binary stars." Thesis, University of St Andrews, 1990. http://hdl.handle.net/10023/14369.

Повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

Анотація:

Spectroscopic and photometric observations of eight contact/near-contact binaries are presented and analysed. Spectroscopic observations were obtained at 4200 Å (radial velocity spectra) and 6563 Å (hydrogen-alpha line profiles). New photometric observations were obtained at visual and infrared wavelengths, and other previously published light curves are also re-analysed. Absolute dimensions have been obtained for five systems; TY Boo, VW Boo, BX And, SS Ari and AG Vir, and their evolutionary positions discussed. Four of the systems are found to be in marginal but poor thermal contact, exhibiting regions of apparent "excess luminosity" in their light curves. A qualitative analysis of these "hot spot" regions has been attempted for the first time using spot models now incorporated into a light curve synthesis programme. Substantial time for this project was awarded on telescopes funded by the United Kingdom Science and Engineering Research Council (SERC), comprising 14 nights at the Issac Newton Telescope (INT) on La Palma, and 4 nights at the United Kingdom Infrared Telescope (UKIRT) on Mauna Kea. Additional observations were made during an 8 night commissioning run on the Jacobus Kapteyn Telescope (JKT) on La Palma, and extensive observations were made with the Twin Photometric Telescope (TPT) at St Andrews University Observatory between 1985 and 1989. These resulted in over 100 spectra at 4200 Å and over 50 spectra at 6563 Å (INT and JKT observations), over 300 infrared photometric observations (UKIRT), and over 3500 visual photometric observations (TPT). Of the five systems analysed in detail in this work, TY Boo appears to be a normal shallow-contact W-type system. Both VW Boo and BX And exhibit regions of "excess luminosity" around the ingress and egress of secondary minimum which are well modelled by a warm spot on the cooler component sitting symmetrically around the neck joining the pair. Such a phenomenon may be expected to arise naturally in systems which have come into contact but are not yet/currently in thermal contact, exhibiting a temperature difference between the components. BXAnd like other B-type systems seems to be reaching this contact state for the first time, but the position of VW Boo is uncertain, and whilst evidence that it could be in the "broken contact" state predicted by the TRO Theory is far from conclusive, its lower orbital angular momentum clearly marks the system as worthy of further study. SS Ari and AG Vir exhibit light curves with unequal quadrature heights. Attempts to treat the higher quadrature as a region of "excess luminosity" due to an energy transfer "warm spot" does not however provide a good model of this phenomenon. Since invoking a dark starspot model also does not provide a good explanation for such systems, it may be that this form of light curve distortion is due to an entirely different form of distorting surface phenomenon. Like BX And, AG Vir appears to be just reaching contact for the first time, but like VW Boo, the slightly lower angular momentum of SS Ari warrants further study.

10

Edwards, Philip Gregory. "A search for ultra high energy gamma ray emission from binary X-ray systems." Title page, contents and summary only, 1988. http://web4.library.adelaide.edu.au/theses/09PH/09phe266.pdf.

Повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

Більше джерел

Книги з теми "Double stars":

1

Swain, Kelley. Double the stars. Blaenau Ffestiniog: Cinnamon Press, 2014.

Знайти повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

2

Jorge, Sahade, McCluskey G. E, and Kondo Yoji, eds. The Realm of interacting binary stars. Dordrecht: Kluwer Academic Publishers, 1993.

Знайти повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

3

Worley, Charles E. Micrometer measures of 2589 double stars. Washington, D.C: U.S. Government Printing Office, 1989.

Знайти повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

4

Walker, Richard L. Micrometer measures of 711 double stars. Washington: U.S. G.P.O., 1985.

Знайти повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

5

International, Conference on Binaries (2010 Mykonos Greece). International Conference on Binaries: In celebration of Ron Webbink's 65th birthday, Mykonos, Greece, 22-25 June 2010. Melville, N.Y: American Institute of Physics, 2010.

Знайти повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

6

United States. National Aeronautics and Space Administration., ed. LSS 2018: A double-lined spectroscopic binary central star with an extremely large reflection effect. [Washington, D.C.?: National Aeronautics and Space Administration?, 1985.

Знайти повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

7

1939-, Milone E. F., Leahy D. A, and Hobill David W, eds. Short-period binary stars: Observations, analyses, and results. [New York?]: Springer Verlag, 2008.

Знайти повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

8

I, Pustylʹnik, ed. Nestat͡s︡ionarnye prot͡s︡essy v tesnykh dvoĭnykh sistemakh: Materialy vsesoi͡u︡znogo soveshchanii͡a︡, Tyravere, 10-14 okti͡a︡bri͡a︡ 1989 g. [Tallinn]: Eesti Teaduste Akadeemia, W. Struve nim. Tartu Astroüüsika Observatoorium, 1989.

Знайти повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

9

United States. National Aeronautics and Space Administration., ed. LSS 2018: A double-lined spectroscopic binary central star with an extremely large reflection effect. [Washington, D.C.?: National Aeronautics and Space Administration?, 1985.

Знайти повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

10

Vanbeveren, D. The brightest binaries. Dordrecht: Kluwer Academic Publishers, 1998.

Знайти повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

Більше джерел

Частини книг з теми "Double stars":

1

van Zyl, J. E. "Stars and Double Stars." In Unveiling the Universe, 157–93. London: Springer London, 1996. http://dx.doi.org/10.1007/978-1-4471-1037-8_10.

Повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

2

Eagle, Dave. "Variable and Double Stars." In The Patrick Moore Practical Astronomy Series, 89–106. New York, NY: Springer New York, 2013. http://dx.doi.org/10.1007/978-1-4614-8766-1_6.

Повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

3

Rakos, K. D., H. A. McAlister, H. A. Abt, P. Couteau, J. Dommanget, M. G. Fracastoro, R. S. Harrington, and A. A. Kiselyov. "Double and Multiple Stars." In Reports on Astronomy, 253–56. Dordrecht: Springer Netherlands, 1988. http://dx.doi.org/10.1007/978-94-009-2981-4_18.

Повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

4

Bergeron, Jacqueline. "Double and Multiple Stars." In Reports on Astronomy, 239–42. Dordrecht: Springer Netherlands, 1994. http://dx.doi.org/10.1007/978-94-011-1100-3_18.

Повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

5

West, Richard M. "Double and Multiple Stars." In Reports on Astronomy, 269–75. Dordrecht: Springer Netherlands, 1985. http://dx.doi.org/10.1007/978-94-009-5392-5_18.

Повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

6

Leverington, David. "Variable and Double Stars." In A History of Astronomy, 154–70. London: Springer London, 1995. http://dx.doi.org/10.1007/978-1-4471-2124-4_8.

Повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

7

Argyle, Bob, and R. W. Argyle. "Why Observe Double Stars?" In Observing and Measuring Visual Double Stars, 17–24. New York, NY: Springer New York, 2012. http://dx.doi.org/10.1007/978-1-4614-3945-5_2.

Повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

8

Argyle, Bob, and R. W. Argyle. "Ten Famous Double Stars." In Observing and Measuring Visual Double Stars, 91–103. New York, NY: Springer New York, 2012. http://dx.doi.org/10.1007/978-1-4614-3945-5_9.

Повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

9

McNally, Derek. "Double and Multiple Stars." In Reports on Astronomy, 243–46. Dordrecht: Springer Netherlands, 1991. http://dx.doi.org/10.1007/978-94-011-3364-7_18.

Повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

10

Argyle, Bob, and R. W. Argyle. "Multiple Stars and Planets." In Observing and Measuring Visual Double Stars, 53–63. New York, NY: Springer New York, 2012. http://dx.doi.org/10.1007/978-1-4614-3945-5_5.

Повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

Тези доповідей конференцій з теми "Double stars":

1

Docobo, J. A., M. Andrade, and P. P. Campo. "Guests in double stars." In INTERNATIONAL WORKSHOP: BINARIES INSIDE AND OUTSIDE THE LOCAL INTERSTELLAR BUBBLE. AIP, 2012. http://dx.doi.org/10.1063/1.4718583.

Повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

2

van den Heuvel, E. P. J. "Double Neutron Stars: Evidence For Two Different Neutron‐Star Formation Mechanisms." In THE MULTICOLORED LANDSCAPE OF COMPACT OBJECTS AND THEIR EXPLOSIVE ORIGINS. American Institute of Physics, 2007. http://dx.doi.org/10.1063/1.2774916.

Повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

3

Indriati, Diari, Widodo, Indah E. Wijayanti, and Kiki A. Sugeng. "On total irregularity strength of star graphs, double-stars and caterpillar." In PROCEEDINGS OF THE 7TH SEAMS UGM INTERNATIONAL CONFERENCE ON MATHEMATICS AND ITS APPLICATIONS 2015: Enhancing the Role of Mathematics in Interdisciplinary Research. AIP Publishing LLC, 2016. http://dx.doi.org/10.1063/1.4940809.

Повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

4

Arenou, F., J. A. Docobo, V. S. Tamazian, and Y. Y. Balega. "Simulating multiple stars in preparation for Gaia." In INTERNATIONAL WORKSHOP ON DOUBLE AND MULTIPLE STARS: DYNAMICS, PHYSICS, AND INSTRUMENTATION. AIP, 2011. http://dx.doi.org/10.1063/1.3597593.

Повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

5

Pourbaix, D., J. A. Docobo, V. S. Tamazian, and Y. Y. Balega. "Screening and modelling the double and multiple stars observed by Gaia." In INTERNATIONAL WORKSHOP ON DOUBLE AND MULTIPLE STARS: DYNAMICS, PHYSICS, AND INSTRUMENTATION. AIP, 2011. http://dx.doi.org/10.1063/1.3597594.

Повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

6

Dewi, J. D. M., Ph Podsiadlowski, and O. R. Pols. "The Ps − e relation of double neutron stars." In THE MULTICOLORED LANDSCAPE OF COMPACT OBJECTS AND THEIR EXPLOSIVE ORIGINS. American Institute of Physics, 2007. http://dx.doi.org/10.1063/1.2774924.

Повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

7

Sinachopoulos, D. "CCD Measurements of Hipparcos Wide Visual Double Stars." In RECENT ADVANCES IN ASTRONOMY AND ASTROPHYSICS: 7th International Conference of the Hellenic Astronomical Society. AIP, 2006. http://dx.doi.org/10.1063/1.2348006.

Повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

8

Docobo, J. A., J. F. Ling, J. A. Docobo, V. S. Tamazian, and Y. Y. Balega. "Binary stars with late-type components: 6 orbits and system masses." In INTERNATIONAL WORKSHOP ON DOUBLE AND MULTIPLE STARS: DYNAMICS, PHYSICS, AND INSTRUMENTATION. AIP, 2011. http://dx.doi.org/10.1063/1.3597589.

Повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

9

Stoica, Sabin, Livius Trache, Alexei Smirnov, and Sabin Stoica. "Introduction to Double Beta Decay." In EXOTIC NUCLEI AND NUCLEAR∕PARTICLE ASTROPHYSICS (III): From Nuclei to Stars. AIP, 2010. http://dx.doi.org/10.1063/1.3527255.

Повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

10

Tamazian, V. S., J. A. Docobo, Yu Yu Balega, N. D. Melikian, E. A. Malogolovets, J. A. Docobo, V. S. Tamazian, and Y. Y. Balega. "EMCCD Speckle Measurements, Differential Photometry and Dynamical Masses of Visual Binary Stars." In INTERNATIONAL WORKSHOP ON DOUBLE AND MULTIPLE STARS: DYNAMICS, PHYSICS, AND INSTRUMENTATION. AIP, 2011. http://dx.doi.org/10.1063/1.3597584.

Повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

Звіти організацій з теми "Double stars":

1

Dutta, Sumit. Locating Double Stars in the UCAC with the WDS Catalog and CCD Parameters. Fort Belvoir, VA: Defense Technical Information Center, July 2008. http://dx.doi.org/10.21236/ada482998.

Повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

2

Mason, Brian D. Various Orbital Solutions and Double Star Statistics. Fort Belvoir, VA: Defense Technical Information Center, October 2011. http://dx.doi.org/10.21236/ada564705.

Повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

3

Zilberman, Mark. Shouldn’t Doppler 'De-boosting' be accounted for in calculations of intrinsic luminosity of Standard Candles? Intellectual Archive, September 2021. http://dx.doi.org/10.32370/iaj.2569.

Повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

Анотація:

"Doppler boosting / de-boosting" is a well-known relativistic effect that alters the apparent luminosity of approaching/receding radiation sources. "Doppler boosting" alters the apparent luminosity of approaching light sources to appear brighter, while "Doppler de-boosting" alters the apparent luminosity of receding light sources to appear fainter. While "Doppler boosting / de-boosting" has been successfully accounted for and observed in relativistic jets of AGN, double white dwarfs, in search of exoplanets and stars in binary systems it was ignored in the establishment of Standard Candles for cosmological distances. A Standard Candle adjustment appears necessary for "Doppler de-boosting" for high Z, otherwise we would incorrectly assume that Standard Candles appear dimmer, not because of "Doppler de-boosting" but because of the excessive distance, which would affect the entire Standard Candles ladder at cosmological distances. The ratio between apparent (L) and intrinsic (Lo) luminosities as a function of redshift Z and spectral index α is given by the formula ℳ(Z) = L/Lo=(Z+1)^(α-3) and for Type Ia supernova as ℳ(Z) = L/Lo=(Z+1)^(-2). These formulas are obtained within the framework of Special Relativity and may require adjustments within the General Relativity framework.

4

Bellwied, R., R. Beuttenmuller, and W. Chen. Double particle resolution in STAR silicon drift detectors. Office of Scientific and Technical Information (OSTI), October 1996. http://dx.doi.org/10.2172/425351.

Повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

5

Lever, James, and Jason Weale. High efficiency fuel sleds for Polar traverses. Engineer Research and Development Center (U.S.), March 2022. http://dx.doi.org/10.21079/11681/43445.

Повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

Анотація:

We describe here the evolution of lightweight, high-efficiency fuel sleds for Polar over-snow traverses. These sleds consist of flexible bladders strapped to sheets of high molecular weight polyethylene. They cost 1/6th, weigh 1/10th and triple the fuel delivered per towing tractor compared with steel sleds. An eight-tractor fleet has conducted three 3400-km roundtrips to South Pole with each travers delivering 320,000 kg of fuel while emitting <1% the pollutants, consuming 1/2 the fuel and saving $1.6 M compared with aircraft resupply. A two tractor fleet in Greenland recently delivered 83,000 kg of fuel in bladder sleds to Summit with similar benefits. Performance monitoring has revealed that bladder-sled towing resistance is largely governed by sliding friction, which can start high and drop in half over the first 30 min of travel. Frictional heating probably produces a thin water layer that lubricates the sled–snow interface. Consequently, towing resistance depends on the thermal budget of the sled. For example, black fuel bladders increase solar gain and thus decrease sled resistance; data suggest they could double again the fuel delivered per tractor. The outstanding efficiency and low cost of these sleds has transformed fuel delivery to Polar research stations.

6

Fitzpatrick, Rachael. Secondary Education Provision and Impacts of Low Secondary Uptake on Wider Societal Outcomes. Institute of Development Studies, August 2022. http://dx.doi.org/10.19088/k4d.2022.122.

Повний текст джерела

Стилі APA, Harvard, Vancouver, ISO та ін.

Анотація:

This report explores the current uptake and completion of secondary education globally, with a particular focus on sub-Saharan Africa. The report also explores the wider societal benefits of increased secondary completion rates, and the financial considerations that are needed to increase uptake and completion. Using data from UIS (2022) and UNESCO WIDE (2022), the report identified disparities in net enrolment, attendance and completion between primary and both levels of secondary education, particularly upper secondary. In sub-Saharan African countries, achievements in net enrolment at primary level are rarely met with high enrolment levels at either lower or upper secondary level, with this difference even more stark when observing completion rates. Currently, both lower and upper secondary education is not a funding priority amongst many countries in sub-Saharan Africa. Of the 27 countries included in analysis, only one country (Mauritius) spent a higher proportion on secondary education compared to other levels (UIS, 2022). Some countries were found to spend a higher proportion of GDP on tertiary education compared to other education levels, with over double the amount spent on tertiary compared to both lower and upper secondary education combined in some instances (Ethiopia, Sierra Leone, South Sudan) (UIS, 2022).