Статті в журналах: "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.

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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.

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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.

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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.

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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.

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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.

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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.

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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.

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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.

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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.

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11

Gondek-Rosińska, D., T. Bulik, S. Osłowski, and K. Belczyński. "Properties of double neutron stars." EAS Publications Series 30 (2008): 137–40. http://dx.doi.org/10.1051/eas:0830015.

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12

Fracastoro, K. G., K. D. Rakos, J. Dommanget, O. G. Franz, W. D. Heintz, H. A. McAlister, A. Poveda, and C. D. Scarfe. "26. Double and Multiple Stars." Transactions of the International Astronomical Union 19, no. 1 (1985): 269–75. http://dx.doi.org/10.1017/s0251107x00006386.

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Commission 26 has changed its name. The new denomination, warmly promoted by Dommanget, represents more adequately the actual field of the Commission Itself and appears as a good start for extending its interest beyond the traditional aspects (morphology and statistics) and plunging into problems connected with the origin, evolution, mass spectrum and dynamics of small star associations.

13

Vilkki, E. U. "Photographic Observations of Double Stars." Publications of the Astronomical Society of the Pacific 101 (December 1989): 1132. http://dx.doi.org/10.1086/132588.

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14

Clarke, D., and P. A. McGale. "Double Periodicity in Be Stars." International Astronomical Union Colloquium 92 (August 1987): 197–99. http://dx.doi.org/10.1017/s0252921100116203.

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SummaryPhotometric periodicities with two unequal maxima and minima reported for Be stars are shown to result from a fundamental and overtone associated with rotation of an atmospheric bulge. It is the form of the scattering function of the free electron that produces the double periodicity; the stellar geometry — co-latitude of the bulge and inclination of the stellar rotational pole — controls the amplitudes of the two components. The form of the light curves is consistent with the oblique rotator model.

15

Fronček, D. "e-Realization of double-stars." Discrete Mathematics 126, no. 1-3 (March 1994): 399–402. http://dx.doi.org/10.1016/0012-365x(94)90285-2.

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16

Pilat-Lohinger, E., B. Funk, and R. Dvorak. "Stability limits in double stars." Astronomy & Astrophysics 400, no. 3 (March 2003): 1085–94. http://dx.doi.org/10.1051/0004-6361:20021811.

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17

Heintz, W. D. "Observations of Double Stars. XVIII." Astrophysical Journal Supplement Series 117, no. 2 (August 1998): 587–98. http://dx.doi.org/10.1086/313127.

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18

Frœschle, M., F. Mignard, and J. L. Falin. "Double Star Recognition." Highlights of Astronomy 9 (1992): 423. http://dx.doi.org/10.1017/s1539299600009412.

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AbstractHipparcos observations provide a wealthy source of discovery of new double and multiple stars. We have developed adequate procedures to recognize in the signal parameters the multiplicity of the stellar source passing through the Hipparcos field of view. These procedures are outlined together with the design of the statistical tests employed. Sampling on real data indicates that about 6000 new double stars will be detected at the mission completion.

19

Tian, Yingzhi, Jixiang Meng, Hong-Jian Lai, and Liqiong Xu. "Connectivity keeping stars or double-stars in 2-connected graphs." Discrete Mathematics 341, no. 4 (April 2018): 1120–24. http://dx.doi.org/10.1016/j.disc.2017.10.017.

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20

Shao, Michael. "Using SIM for Double Star Astronomy." Proceedings of the International Astronomical Union 2, S240 (August 2006): 54–58. http://dx.doi.org/10.1017/s1743921307003791.

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AbstractThe SIM (Planet Quest) mission is a space-based long-baseline stellar interferometer designed for ultra-precise astrometry. This paper describes how SIM can be used for double star research. There are several regimes of operation. For binary stars separated by more than 1″.5, SIM treats these as distinct objects. Double stars less than ∼10 milliarcsec in separation are seen as a single object and SIM measures the photocenter of the composite object. Between 10 mas and 1″.15, SIM is able to see the double star as two distinct objects, but because photons from both stars are detected there is the possibility of increased noise and measurement bias. This paper describes how double stars are observed with SIM and what information can be derived.

21

Clement, Christine M., James M. Nemec, Robert J. Dickens, and Elizabeth A. Bingham. "Double-Mode RR Lyrae Stars in IC 4499." Symposium - International Astronomical Union 126 (1988): 591–92. http://dx.doi.org/10.1017/s0074180900043229.

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Thirteen double-mode RR Lyrae (RRd) stars, with mean magnitudes c = 18.30 ± 0.10 and <V>c = 17.80 ± 0.15, have been identified in the variable-rich Oosterhoff type I globular cluster IC 4499. The stars have surprisingly uniform properties, and are considerably different from RRd stars found in Oo II systems. The mean first-overtone period (Fig.1) is <P1>=0.357d ± 0.005d (cf. <P1>=0.40d for Oo II RRd stars), and the mean ratio of the first-overtone period to the fundamental period is <P1/P0>= 0.7443 ± 0.0002. The mean double-mode pulsation mass for the 13 stars, using the King Ia (Y=0.279, Z=0.001) mass calibration, is 0.535 ± 0.003 M⊙. Such an average mass is 0.11 M⊙ smaller (i.e. ~17% smaller) than that for RRd stars found in Oo II systems, and possibly ~0.01 M⊙smaller than the mean mass for the two RRd stars in M3 (it is important to note that the zero point of these mass determinations is uncertain by at least 15%). The metal abundances for the RRd stars, and for the system of RR Lyrae stars as a whole, are found to be consistent with <[Fe/H]>=-1.38 ± 0.20, determined from δS spectroscopy. In the Peterson diagram (Fig.2), all known RRd stars now divide (apparently by mass) into two groups (split according to Oosterhoff type). With a reddening of EB-V=0.26 ± 0.03, the cluster distance modulus is (m-M)o=16.23m ± 0.23m.

22

Scarfe, C. D., W. I. Hartkopf, J. T. Armstrong, F. C. Fekel, P. Lampens, J. F. Ling, R. D. Mathieu, M. J. Valtonen, and H. Zinnecker. "Commission 26: Double and Multiple Stars (Etoiles Doubles Et Multiples)." Transactions of the International Astronomical Union 25, no. 1 (2002): 224–29. http://dx.doi.org/10.1017/s0251107x00001462.

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23

Olevic, D., G. Popovic, and P. Jovanovic. "Recalculated orbits of 8 double stars." Serbian Astronomical Journal, no. 162 (2000): 109–13. http://dx.doi.org/10.2298/saj0062109o.

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The authors present new orbital elements for the following pairs: ADS 1227 ADS 3317, ADS 8128, ADS 8239, ADS 8242, ADS 8539, ADS 8949 and McA 61. Individual masses for these pairs are also calculated. For the pairs ADS 8128, ADS 8239, ADS 8539 and ADS 8949 calculated parallaxes are in accordance with the corresponding parallaxes of the Hipparchos Program.

24

McCarthy, C., B. Zuckerman, and E. E. Becklin. "Discovery of 14 Nearby Double Stars." Astronomical Journal 121, no. 6 (June 2001): 3259–65. http://dx.doi.org/10.1086/321076.

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25

Docobo, J. A., J. F. Ling, and C. Prieto. "Orbits of six visual double stars." Astrophysical Journal Supplement Series 91 (April 1994): 793. http://dx.doi.org/10.1086/191955.

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26

Osłowski, S., T. Bulik, D. Gondek-Rosińska, and K. Belczyński. "Population synthesis of double neutron stars." Monthly Notices of the Royal Astronomical Society 413, no. 1 (January 31, 2011): 461–79. http://dx.doi.org/10.1111/j.1365-2966.2010.18147.x.

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27

Lau, Mike Y. M., Ilya Mandel, Alejandro Vigna-Gómez, Coenraad J. Neijssel, Simon Stevenson, and Alberto Sesana. "Detecting double neutron stars with LISA." Monthly Notices of the Royal Astronomical Society 492, no. 3 (January 10, 2020): 3061–72. http://dx.doi.org/10.1093/mnras/staa002.

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ABSTRACT We estimate the properties of the double neutron star (DNS) population that will be observable by the planned space-based interferometer Laser Interferometer Space Antenna (LISA). By following the gravitational radiation-driven evolution of DNSs generated from rapid population synthesis of massive binary stars, we estimate that around 35 DNSs will accumulate a signal-to-noise ratio above 8 over a 4-yr LISA mission. The observed population mainly comprises Galactic DNSs (94 per cent), but detections in the LMC (5 per cent) and SMC (1 per cent) may also be expected. The median orbital frequency of detected DNSs is expected to be 0.8 mHz, and many of them will be eccentric (median eccentricity of 0.11). LISA is expected to localize these DNSs to a typical angular resolution of 2°. We expect the best-constrained DNSs to have eccentricities known to a few parts in a thousand, chirp masses measured to better than 1 per cent fractional uncertainty, and sky localization at the level of a few arcminutes. The orbital properties will provide insights into DNS progenitors and formation channels. The localizations may allow neutron star natal kick magnitudes to be constrained through the Galactic distribution of DNSs, and make it possible to follow up the sources with radio pulsar searches. LISA is also expected to resolve ∼104 Galactic double white dwarfs, many of which may have binary parameters that resemble DNSs; we discuss how the combined measurement of binary eccentricity, chirp mass, and sky location may aid the identification of a DNS.

28

Allen, Christine, Jose A. D. Docobo, William I. Hartkopf, Yuri I. Balega, John Davis, Brian D. Mason, Edouard Oblak, Terry D. Oswalt, Dimitri Pourbaix, and Colin D. Scarfe. "COMMISSION 26: DOUBLE AND MULTIPLE STARS." Proceedings of the International Astronomical Union 4, T27A (December 2008): 196–206. http://dx.doi.org/10.1017/s1743921308025519.

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Although we were happy to welcome over 20 new members at the Prague meeting, Commission 26 is still one of the smallest in the IAU. Notwithstanding its size, it continues to carry on an active and diversified program of activities. Our web site, maintained at the US Naval Observatory, contains further information on the Commission. The site includes links to other relevant sites, to databases and catalogues, an archive of our Information Circulars, a list of upcoming meetings of interest, as well as an extensive bibliography of recently published papers on double and multiple stars. The site can be accessed at <ad.usno.navy.mil/wds/dsl.html#iau>.

29

Rakos, K. D., H. A. McAlister, H. A. Abt, P. Couteau, M. G. Fracastoro, R. S. Harrington, and A. A. Kiselyov. "Commission 26: Double and Multiple Stars." Transactions of the International Astronomical Union 20, no. 1 (1988): 253–56. http://dx.doi.org/10.1017/s0251107x00007185.

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In the recent years new techniques are expanding visual binary star astronomy into previously inaccessible regimes of angular resolution and accuracy of measurements regarding the astrometric and astrophysical parameters of their components. New techniques and algorithms are providing enhanced sensitivity to low mass companions and the determination of photometric properties of the components of close visual binaries. The potential now exists for significantly narrowing, if not eliminating entirely, the historic gap separating spectroscopic from visual binaries. Advances in closely related fields as in precision radial velocity measurement and enhanced accuracy of parallax determination from ground and space based observatories will place demands upon double star astronomy that have been absent for half a century. Today double and multiple star astronomy is perhaps closer to fulfilling its true potential than it has ever been, entering a fundamentally important area of modern astrophysics.

30

McAlister, H. A. "Commission 26 : Double and Multiple Stars." Transactions of the International Astronomical Union 21, no. 1 (1991): 243–46. http://dx.doi.org/10.1017/s0251107x00010075.

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The observational study of double and multiple stars is traditionally seen as comprised of several specialized subfields, each defined by particular observational selection effects. Improvements in increased precision and accuracy, higher resolution, higher signal-to-noise ratios, greater sensitivity etc.), are leading the study of double stars to a truly coherent field. Significant advances in ground-based spectroscopy and interferometry provide a framework from which we can prepare for the future. The contributions to be made from space are currently in a state of uncertainty as we await results from the Hubble Space Telescope and Hipparcos.

31

Sinachopoulos, D., and P. Mouzourakis. "Searching for Optical Visual Double Stars." International Astronomical Union Colloquium 135 (1992): 252–54. http://dx.doi.org/10.1017/s0252921100006515.

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AbstractWe study a sample of 123 wide visual double stars for which astrophysical parameters are at least partly available from uvby Hβ photometry. All of these have components brighter than 10 mags and a component angular separation between 10 and 20 arcseconds.We find that at least one third of them are optical; for relative proper motion (RPM) pairs this fraction is 60% or even more. These results are in fair agreement with the predictions we formulated in an earlier paper on the basis of a statistical criterion.

32

Hartkopf, William I., Christine Allen, J. A. Davis, F. C. Fekel, P. Lampens, J. F. Ling, E. Oblak, T. D. Oswalt, and C. Scarfe. "Commission 26: Double and Multiple Stars." Proceedings of the International Astronomical Union 1, T26A (December 2005): 193–202. http://dx.doi.org/10.1017/s1743921306004546.

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While Commission 26 remains one of the smallest in the IAU, it maintains an active program which belies its size, as highlighted below. Further information on the commission may be found at our website: http://ad.usno.navy.mil/wds/dsl.html\#iau. This site includes links to other sites and to major databases and catalogues, as well as bibliographies of recent double star papers, an archive of the Commission's Information Circulars, and a list of upcoming meetings.

33

Allen, Christine, Jose A. Docobo, William I. Hartkopf, Yuri I. Balega, John Davis, Brian D. Mason, Edouard Oblak, Terry D. Oswalt, Dimitri Pourbaix, and Colin D. Scarfe. "COMMISSION 26: DOUBLE AND MULTIPLE STARS." Proceedings of the International Astronomical Union 6, T27B (May 14, 2010): 191–92. http://dx.doi.org/10.1017/s174392131000503x.

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The business meeting of Commission 26 was held on Friday, 7 August 2009, and consisted mainly of scientific talks. At the end, incoming President J. A. Docobo gave a video presentation with his thoughts regarding future activities of Commission 26, including the comments of members of the OC. He also announced a December 2009 workshop and discussed potential meetings in the coming years.

34

Docobo, Jose A., Brian D. Mason, Christine Allen, Frederic Arenou, Yuri Balega, Terry Oswalt, Dimitri Pourbaix, Marco Scardia, Colin Scarfe, and Vakhtang S. Tamazian. "COMMISSION 26: DOUBLE AND MULTIPLE STARS." Proceedings of the International Astronomical Union 7, T28A (December 2011): 150–56. http://dx.doi.org/10.1017/s174392131200275x.

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35

Kamper, K. W. "Photographic measurements of southern double stars." Publications of the Astronomical Society of the Pacific 97 (June 1985): 579. http://dx.doi.org/10.1086/131571.

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36

Chruslinska, Martyna, Krzysztof Belczynski, Jakub Klencki, and Matthew Benacquista. "Double neutron stars: merger rates revisited." Monthly Notices of the Royal Astronomical Society 474, no. 3 (November 14, 2017): 2937–58. http://dx.doi.org/10.1093/mnras/stx2923.

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37

Worley, Charles E. "Double Stars In The Astrographic Catalogue." Symposium - International Astronomical Union 133 (1988): 491–95. http://dx.doi.org/10.1017/s0074180900140094.

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Nearly 20000 double stars have been detected from star positions listed in the Astrographic Catalogue. However, an examination of the various discoverer's efforts reveals that the past searches have been very incomplete. In fact, if the limits adopted by one discoverer were applied to the remainder of the catalogue, approximately 3·105 additional pairs would be found. Is such an endeavor justifiable scientifically?

38

Batten, A. H. "Spectroscopic observations of visual double stars." Symposium - International Astronomical Union 118 (1986): 425–27. http://dx.doi.org/10.1017/s0074180900151800.

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39

Docobo, J. A., and J. F. Ling. "Orbits of Five Visual Double Stars." Astrophysical Journal Supplement Series 120, no. 1 (January 1999): 41–48. http://dx.doi.org/10.1086/313166.

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40

Alzner, A. "Measurements of double stars 1993.67 - 1998.13." Astronomy and Astrophysics Supplement Series 132, no. 2 (October 1998): 237–52. http://dx.doi.org/10.1051/aas:1998291.

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41

Jasinta, D. M. D., M. Raharto, and E. Soegiartini. "Photographic observations of visual double stars." Astronomy and Astrophysics Supplement Series 134, no. 1 (January 1999): 87. http://dx.doi.org/10.1051/aas:1999121.

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42

Mignard, F., M. Badiali, P. L. Bernacca, H. Bernstein, D. Cardini, A. Emanuele, J. L. Falin, M. Froeschlé, R. Hering, and G. Prezioso. "HIPPARCOS First Results in the Double Star Processing by the FAST Consortium." International Astronomical Union Colloquium 135 (1992): 403–11. http://dx.doi.org/10.1017/s0252921100006886.

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AbstractAfter the processing of one year of observations carried out by HIPPARCOS it is possible to provide quantitative results as to the number of new double and multiple stars to be detected and the real capacity of this mission to perform relative astrometry on double stars. We present and discuss the methods developed to this end and include the first results concerning the detection statistics and the determination of separation and position angle for double stars. About 16,000 stars have been recognized as non-single, including 9,000 already known as double and mutliple before the mission. Also, a subset of 10,500 stars have been successfully solved for their relative coordinates with an accuracy in the range of 3 to 10 mas.

43

Dommanget, J., and O. Nys. "The Catalogue of the Components of Double and Multiple Stars (CCDM) - First Edition." Symposium - International Astronomical Union 166 (1995): 395. http://dx.doi.org/10.1017/s0074180900228714.

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The Hipparcos mission required the realisation of an Input Catalogue giving the positions of 100.000 stars (single or components of double and multiple systems) to an accuracy better than 1″5. At the start of this work (1981) no specific catalogue of double and multiple stars provided these data. The only general data base on double stars available to us, giving positions to ±1′, was the Index (1961,0) updated at the USNO by C. E. Worley till 1976,5 and of which a copy was communicated by P. Muller of the Observatoire de Meudon. It has then been decided to reformat this Catalogue in such a way as to allow the introduction of all necessary information for the mission. This permitted a correct cross-identification with the Hipparcos Input Catalogue (of finally 118.000 stars). It was later called: the Catalogue of the Components of Double and Multiple stars (CCDM). Since then, it has been developed and its aim remains to furnish the best accurate locations and descriptions of the double and multiple systems on the sky for all double and multiple star research.

44

Mignard, F. "Double Star Astrometry with the Hipparcos Data." Symposium - International Astronomical Union 166 (1995): 69–76. http://dx.doi.org/10.1017/s0074180900227861.

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As we approach the final processing of the observations carried out by HIPPARCOS, in particular for the double and multiple stars, it is possible to provide reliable statistics on the number of such objects detected and on the quality of the relative and absolute astrometry and photometry. About 24 000 stars have been recognized as non-single, including 11 000 already known as double and multiple before the mission and 13000 discovered by Hipparcos. Also, a subset of 16 000 stars among the 24 000 have been successfully solved for their relative coordinates (position angle and separation) with an accuracy in the range of 3 to 30 mas, including 7000 new double stars. I outline in this paper the principle of the internal recognition procedure and present some statistics on the solution.

45

Bauer, Christina, Graeme L. White, David L. Blank, Alex Hons, and Paul A. Jones. "Astrometric Observations of Wide Southern Double Stars – II." Publications of the Astronomical Society of Australia 24, no. 3 (2007): 118–37. http://dx.doi.org/10.1071/as07023.

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AbstractAstrometric CCD observations have been made of wide (∼3 to 60 arcsec) southern double stars selected from the Washington Double Star catalogue (WDS). Southern double stars have not been well studied in the past; typically they had not been measured since about 1930, and ∼50% of them have been observed only once before our observations. Of the pairs measured ∼80% show no evidence of motion since the last observation. This is Paper II in which we present the observations of 290 WDS stars in the approximate RA range 17h 13m to 07h 30m and in the declination range −70° to −60°. We suggest 412 companions for these 290 stars and list 29 (10%) pairs that have shown significant motion.

46

Foss, Diana. "Three Double Degenerate Candidates." International Astronomical Union Colloquium 114 (1989): 163–66. http://dx.doi.org/10.1017/s0252921100099516.

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This poster reports the results of a search for variable radial velocities in 29 DA white dwarfs. The survey was sensitive to periods between 1h and 66d, although non-ideal sampling limited the longest practically detectable period to 2d. Three stars were discovered to have radial velocity shifts at above the 3σ level. The discovery of these stars, along with that of Saffer, et al. (1988) can put only a lower limit on the space density of close binary white dwarfs, as this survey was less than 100% efficient in detecting radial velocity variations, and its efficiency depended strongly on period.

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Mignard, F., J. L. Falin, and M. Froeschlé. "HIPPARCOS First Results in the Double Star Photometry." International Astronomical Union Colloquium 135 (1992): 421–28. http://dx.doi.org/10.1017/s0252921100006904.

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AbstractIn addition to its astrometric capabilities the HIPPARCOS main detector proves to be a good phototometer. The main features of the photometric reduction applied to double stars are outlined. We show how it is possible to discriminate single stars from multiple stars from the photometric signal. Results presented are based on about 16000 stars recognized as non-single, of which 8000 were not known to be double in the HIPPARCOS Input Catalogue. Magnitudes for multiple systems as a whole are derived with a precision usually better than 0.005 mag while the magnitude of each component is recovered up to magnitude difference of 3 mag, but with less accuracy and precision.

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Halbwachs, Jean–Louis. "First Double Star Observations in the HIPPARCOS Tycho Project." International Astronomical Union Colloquium 135 (1992): 429–34. http://dx.doi.org/10.1017/s0252921100006916.

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AbstractThe Tycho project will provide positions and (B, V) magnitudes for about 1 million stars, and will be complete for stars brighter than magnitude (B + V)/2 = 10.5. The components of double stars will obtain individual measurements when the separations are wider than 3″.

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Denoyelle, J., C. Aerts та C. Waelkens. "Main-sequence broadening, Be stars, and stellar rotation inhand χ Persei". Symposium - International Astronomical Union 162 (1994): 151–52. http://dx.doi.org/10.1017/s0074180900214757.

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The double cluster h andxPersei is one of the richest clusters containing early-B stars, and therefore is important for observational and theoretical studies on the fundamental parameters of massive stars. The colour-magnitude diagram of the double cluster shows an important scatter (see Figure 1). It has long been known thathandxPersei are extremely rich in Be stars (Slettebak 1968). Our previous contention (Waelkens et al. 1990) that the large-amplitude variable stars we discovered are also Be stars, could be confirmed for a few objects. Rotation velocities for stars inhandxPersei are usually high, which is not surprising in view of the large fraction of Be stars.

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Sinachopoulos, D., and E. L. van Dessel. "UBV photometry of wide visual double stars. V. Double stars with mainly K- and M- type primaries." Astronomy and Astrophysics Supplement Series 119, no. 3 (November 1996): 483–88. http://dx.doi.org/10.1051/aas:1996260.

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