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Artículos de revistas sobre el tema "Double stars"

Autor: Grafiati

Publicado: 4 de junio de 2021

Última modificación: 25 de julio de 2025

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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 (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

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4

Agati, Jean-Louis, Sébastien Caille, André Debackère, et al. "Activities and Achievements of the Double Star Committee of the Société Astronomique de France." Proceedings of the International Astronomical Union 2, S240 (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 (s

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5

Rezaei, Zeinab. "Double dark matter admixed neutron star." International Journal of Modern Physics D 27, no. 16 (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.

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6

Zinnecker, H., C. Scarfe, C. Allen, et al. "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

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7

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.

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8

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.

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9

Jia, Qi, Xiaodian Chen, Shu Wang, Licai Deng, Yangping Luo та Qingquan Jiang. "Multimode δ Sct stars from the Zwicky Transient Facility Survey". Astrophysical Journal Supplement Series 273, № 1 (2024): 7. http://dx.doi.org/10.3847/1538-4365/ad4da6.

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Abstract We obtain the largest catalog of multimode δ Sct stars in the northern sky to date using the Zwicky Transient Facility (ZTF) Data Release 20. The catalog includes 2254 objects, of which 2181 are new to our study. Among these multimode δ Sct stars, 2142 objects are double-mode δ Sct, while 109 objects are triple-mode δ Sct and three are quadruple-mode δ Sct. By analyzing the light curves in the r and g bands of the ZTF, we determine the basic parameters of multimode δ Sct stars, including the periods and amplitudes. Periods are checked by comparison with the Optical Gravitational Lensi

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10

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

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11

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.

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12

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

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13

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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14

Fracastoro, K. G., K. D. Rakos, J. Dommanget, et al. "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.

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15

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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16

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.

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17

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

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18

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

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19

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

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20

Tenn, Joseph S. "KEEPERS OF THE DOUBLE STARS." Journal of Astronomical History and Heritage 16, no. 1 (2013): 81–93. http://dx.doi.org/10.3724/sp.j.1440-2807.2013.01.06.

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21

Mignard, F., M. Badiali, P. L. Bernacca, et al. "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 missi

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22

Shao, Michael. "Using SIM for Double Star Astronomy." Proceedings of the International Astronomical Union 2, S240 (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 the

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23

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 th

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24

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

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25

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 usuall

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26

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 (2018): 1120–24. http://dx.doi.org/10.1016/j.disc.2017.10.017.

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27

Cvetkovic, Zorica, R. Pavlovic, and S. Boeva. "CCD measurements of double and multiple stars at NAO Rozhen. IV." Serbian Astronomical Journal, no. 180 (2010): 103–7. http://dx.doi.org/10.2298/saj1080103c.

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Using the 2 m telescope of the Bulgarian National Astronomical Observatory at Rozhen observations of 30 double or multiple stars were carried out during two half nights on July 20 and 21, 2009. This is the fourth series of measurements of CCD frames of double and multiple stars obtained at Rozhen. In this paper we present the results for the position angle and separation for 23 double and 5 multiple stars (35 pairs) which could have been measured.

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28

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

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29

Jia, Qi, Xiaodian Chen, Shu Wang, Licai Deng, Jianxing Zhang та Qingquan Jiang. "Period–Luminosity Relations for Double-mode δ Sct Stars". Astrophysical Journal 984, № 1 (2025): 89. https://doi.org/10.3847/1538-4357/adc685.

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Abstract Previous studies of the period–luminosity relations (PLRs) of Delta Scuti (δ Sct) stars have focused on those with a single pulsation mode. However, for δ Sct stars with many different pulsation modes, classifying a single mode is difficult. In this study, an all-sky data set is constructed using double-mode δ Sct stars from the Zwicky Transient Facility and Optical Gravitational Lensing Experiment and is used to determine fundamental (F)-mode and first-overtone (1O)-mode PLRs for eight single bands and six Wesenheit bands. In the W1 band, the PLR dispersion is about 0.171 mag, and th

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30

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

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31

Scarfe, C. D., W. I. Hartkopf, J. T. Armstrong, et al. "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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32

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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33

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 re

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34

Orlov, V. G. "SPECKLE INTERFEROMETRY AT THE OBSERVATORIO ASTRONÓMICO NACIONAL. VII." Revista Mexicana de Astronomía y Astrofísica 57, no. 1 (2021): 67–80. http://dx.doi.org/10.22201/ia.01851101p.2021.57.01.04.

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The results of speckle interferometric measurements of binary stars performed during June, 2016 with the 2.1 m telescope at the Observatorio Astron&oacute;mico Nacional at SPM (México) are given. We report 480 astrometric measurements of 468 double stars systems. The measured angular separations ρ range from 0’’.091 to 5’’.93. Most of the observed pairs (414 out of 468) are close double stars having separations of ρ ≤ 1’’. We confirm as double stars 59 targets and we found 3 new pairs with separation of less than 1’’. Finally, we show that the high resolution autocorrelation function in po

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35

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 perio

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36

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.

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37

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

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38

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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39

Ruotolo, Jake, and Zi-Xia Song. "Multicolor Ramsey number for double stars." Discrete Mathematics 347, no. 7 (2024): 114034. http://dx.doi.org/10.1016/j.disc.2024.114034.

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40

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 (2011): 461–79. http://dx.doi.org/10.1111/j.1365-2966.2010.18147.x.

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41

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 (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 f

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42

Allen, Christine, Jose A. D. Docobo, William I. Hartkopf, et al. "COMMISSION 26: DOUBLE AND MULTIPLE STARS." Proceedings of the International Astronomical Union 4, T27A (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 c

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43

Rakos, K. D., H. A. McAlister, H. A. Abt, et al. "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 fie

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44

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 res

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45

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.

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46

Hartkopf, William I., Christine Allen, J. A. Davis, et al. "Commission 26: Double and Multiple Stars." Proceedings of the International Astronomical Union 1, T26A (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.

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Allen, Christine, Jose A. Docobo, William I. Hartkopf, et al. "COMMISSION 26: DOUBLE AND MULTIPLE STARS." Proceedings of the International Astronomical Union 6, T27B (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.

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48

Docobo, Jose A., Brian D. Mason, Christine Allen, et al. "COMMISSION 26: DOUBLE AND MULTIPLE STARS." Proceedings of the International Astronomical Union 7, T28A (2011): 150–56. http://dx.doi.org/10.1017/s174392131200275x.

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49

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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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 (2017): 2937–58. http://dx.doi.org/10.1093/mnras/stx2923.

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