sro_research


	SRO Research CBET'S Central Bureau for Astronomical Telegrams INTERNATIONAL ASTRONOMICAL UNION M.S. 18, Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A. IAUSUBS@CFA.HARVARD.EDU or FAX 617-495-7231 (subscriptions) CBAT@CFA.HARVARD.EDU (science) URL http://cfa-www.harvard.edu/iau/cbat.html (5477) 1989 UH_2 B. D. Warner, Palmer Divide Observatory, Colorado Springs; P. Pravec and P. Kusnirak, Ondrejov Observatory; W. Cooney, J. Gross, and D. Terrell, Sonoita Research Observatory, Sonoita, AZ; D. Higgins, Ngunnawal, Canberra, Australia; L. Kornos and J. Vilagi, Modra Observatory; D. Pray, Greene, RI; G. Masi, Universita degli Studi di Roma "Tor Vergata"; and F. Mallia, Campo Catino, Italy, report that observations obtained during Nov. 2-12 show that the minor planet (5477) is a binary system with an orbital period of 24.42 +/- 0.02 hr. The primary rotates with a period of 2.9943 +/- 0.0002 hr, and its lightcurve amplitude of 0.11 mag indicates a nearly spherical shape. Mutual eclipse/occultations events that are 0.14-0.22 mag deep indicate a secondary-to-primary mean-diameter ratio of 0.37 +/- 0.02. Follow-up observations in the next lunation are desirable. NOTE: These 'Central Bureau Electronic Telegrams' are sometimessuperseded by text appearing later in the printed IAU Circulars. (C) Copyright 2005 CBAT2005 November 15 (CBET 288)Daniel W. E. Green (3309) BRORFELDE B. D. Warner, Palmer Divide Observatory, Colorado Springs ; P.Pravec and P. Kusnirak, Ondrejov Observatory; W. Cooney, J. Gross, and D. Terrell, Sonoita Research Observatory, Sonoita , AZ ; and S. Nudds, Elginfield Observatory, University of Western Ontario , report that photometric observations obtained from Oct. 25 to Nov. 3 show that the minor planet (3309) is a binary system with an orbital period of 18.48 +/- 0.01 hr. The primary rotates with a period of 2.5041 +/- 0.0002 hr, and its lightcurve amplitude of 0.09 mag indicates a nearly spheroidal shape. Mutual eclipse/occultations events that are 0.07-0.15 mag deep indicate a secondary-to-primary mean-diameter ratio of 0.26 +/- 0.02. Calibrated data gives an estimated absolute magnitude H_R = 13.4 +/- 0.2, assuming G = 0.15+/- 0.2. NOTE: These 'Central Bureau Electronic Telegrams' are sometimessuperseded by text appearing later in the printed IAU Circulars. (C) Copyright 2005 CBAT2005 November 7(CBET 279)Daniel W. E. Green (9260) EDWARDOLSON M. Jakubik and M. Husarik, Skalnate Pleso Observatory; J. Vilagi, S. Gajdos, and A. Galad, Modra Observatory; P. Pravec and P. Kusnirak, Ondrejov Observatory; W. Cooney, J. Gross and D. Terrell via Sonoita Research Observatory (Sonoita, AZ); D. Pray, Greene, RI; and R. Stephens, Yucca Valley, CA, report that photometric observations obtained during Oct. 6-30 show that the minor planet (9260) is a binary system with an orbital period of 17.785 +/- 0.003 hr. The primary rotates with a period of 3.0852 +/- 0.0001 hr, and its lightcurve amplitude of0.11 mag is indicative of a nearly spheroidal shape. Mutual eclipse/occultation events that are 0.08-0.15 mag deep indicate a secondary-to-primary mean-diameter ratio of 0.27 +/- 0.03. NOTE: These 'Central Bureau Electronic Telegrams' are sometimessuperseded by text appearing later in the printed IAU Circulars. (C) Copyright 2005 CBAT 2005 November 2 (CBET 270) Daniel W. E. Green (2044) Wirt D. Pray, Carbuncle Hill Observatory, Greene, RI; P. Pravecand P. Kusnirak, Ondrejov Observatory; W. Cooney, J. Gross, andD. Terrell, Sonoita Research Observatory, Sonoita, AZ; A. Galad,S. Gajdos, and J. Vilagi, Modra Observatory; and R Durkee,Minneapolis, MN, report that photometric observations obtainedduring 2005 Dec. 8-29 reveal that minor planet (2044) is a binarysystem with an orbital period of 18.97 ± 0.01 hr. The primaryrotates with a period of 3.6898 ± 0.0001 hr, and its lightcurveamplitude is 0.26 mag. Mutual eclipse/occultations events thatare 0.07- to 0.15-mag deep indicate a secondary-to-primarymean-diameter ratio of 0.25 ± 0.02. NOTE: These 'Central Bureau Electronic Telegrams' are sometimes superseded by text appearing later in the printed IAU Circulars. (C) Copyright 2006 CBAT 2006 January 6 (CBET 353) Daniel W. E. Green" (1717) ARLON W. Cooney, J. Gross, and D. Terrell, Sonoita Research Observatory, Sonoita, AZ; R. Stephens, Yucca Valley, CA; P. Pravec and P. Kusnirak, Ondrejov Observatory; R. Durkee, Minneapolis, MN; and A. Galad, Modra Observatory, report that photometric observations obtained during 2005 Dec. 4-2006 Jan. 11 reveal that minor planet (1717) has a lightcurve consisting of two linearly additive components with periods 5.1484 and 18.236 hr (and amplitudes 0.08 and 0.13 mag), respectively. Attenuations due to occultations/eclipses do not appear to be occurring at the present geometry, but further monitoring through the end of the current apparition and at future apparitions (to look for attenuations at different geometries) are needed to confirm the inferred binary nature and determine the relative sizes of the components. (C) Copyright 2006 CBAT 2006 January 17 ( CBET 369) Daniel W. E. Green (4029) BRIDGES D. Higgins, Canberra, Australia; P. Pravec and P. Kusnirak, Ondrejov Observatory; W. Cooney, J. Gross, and D. Terrell, Sonoita Research Observatory, Sonoita, AZ; and R. Stephens, Yucca Valley, CA, report that photometric observations obtained during Apr. 11-May 4 reveal that minor planet (4029) is a binary system with an orbital period of 16.31 ± 0.01 hours. The primary rotates with a period of 3.5746 ± 0.0001 hours, and it has a lightcurve amplitude of 0.20 mag. Mutual eclipse/occultation events that are 0.06-0.12 mag deep indicate a secondary-to-primary mean-diameter ratio of 0.24 ± 0.02. NOTE: These 'Central Bureau Electronic Telegrams' are sometimessuperseded by text appearing later in the printed IAU Circulars. (C) Copyright 2006 CBAT 2006 May 8 (CBET 507) Daniel W. E. Green (3073) KURSK P. Kusnirak and P. Pravec, Ondrejov Observatory; S. Gajdos and A.Galad, Modra Observatory; W. Cooney, J. Gross, and D. Terrell, Sonoita Research Observatory, Sonoita, AZ; D. Pray, Carbuncle Hill Observatory, Greene, RI; F. Colas and J. Lecacheux, Pic du Midi Observatory; V. Reddy, Department of Earth System Science and Policy, University of North Dakota, Grand Forks; and R. Dyvig, Quinn, SD, report that photometric observations obtained during 2006 Dec. 11-27 reveal that minor planet(3073) is a binary system with an orbital period of 44.96 ± 0.02 hr. The primary shows a period of 3.4468 ± 0.0001 hr, and it has a lightcurve amplitude of 0.21 mag. Mutual eclipse/occultation events that are 0.06- to 0.07-mag deep indicate a secondary-to-primary mean-diameter ratio of 0.25 ± 0.02. NOTE: These 'Central Bureau Electronic Telegrams' are sometimessuperseded by text appearing later in the printed IAU Circulars. (C) Copyright 2007 CBAT 2007 January 3 (CBET 792) Daniel W. E. Green (2486) METSAHOVI M. Pikler, M. Husarik, and G. Cervak, Skalnate Pleso Observatory; W. Cooney, J. Gross, and D. Terrell, Sonoita Research Observatory, Sonoita, AZ; P. Pravec and P. Kusnirak, Ondrejov Observatory; A. Galad, J. Vilagi, L. Kornos, and S. Gajdos, Modra Observatory; V. Reddy, Department of Earth System Science and Policy, University of North Dakota, Grand Forks; and R.Dyvig, Quinn, SD, report that photometric observations obtained during 2006 Dec. 12 to 2007 Jan. 26 reveal that (2486) has a lightcurve consisting of two linearly additive components with periods 4.4518 and 2.6404 hr and amplitudes 0.12 and 0.04 mag, respectively. No attenuations due to occultations/eclipses were seen, so the proposed interpretation of binary nature of the minor planet needs to be confirmed with further observations. The mean absolute R magnitude in the Cousins system is 12.14 ± 0.2, assuming G = 0.15 ± 0.2. NOTE: These 'Central Bureau Electronic Telegrams' are sometimessuperseded by text appearing later in the printed IAU Circulars. (C) Copyright 2007 CBAT 2007 February 26 (CBET 860) Daniel W. E. Green (8116) JEANPERRIN D. Higgins, Canberra, Australia; P. Pravec, P. Kusnirak, and K. Hornoch, Ondrejov Observatory; M. Husarik, M. Pikler, and G. Cervak, Skalnate Pleso Observatory; D. Pray, Carbuncle Hill Observatory, Greene, RI; S. Gajdos, Modra Observatory; Yu. Krugly, Institute of Astronomy, Kharkiv National University, National Academy of Science of Ukraine; A. Marshalkina, Ulugh Beg Astronomical Institute, Uzbek Academy of Sciences; R. Stephens, Goat Mountain Astronomical Research Station, Yucca Valley, CA; F. Colas, Pic du Midi Observatory; and W. Cooney, J. Gross, and D. Terrell, Sonoita Research Observatory, Sonoita, AZ, report that photometric observations obtained during Oct. 4-Nov. 7 reveal that minor planet (8116) is a binary system with an orbital period of 36.15 ± 0.02 hr. The primary shows a period of 3.6169 ± 0.0002 hr, and it has a lightcurve amplitude of 0.09 mag, suggesting a nearly spheroidal shape. Mutual eclipse/occultation events indicate a lower limit on the secondary-to-primary mean-diameter ratio of 0.33. Calibrated data give an estimated mean absolute magnitude H_R = 13.52 ± 0.13, assuming G = 0.15 ± 0.2. (C) Copyright 2007 CBAT 2007 November 9 (CBET 1127) Daniel W. E. Green (16635) 1993 QO D. Pray, Carbuncle Hill Observatory, Greene, RI; P. Pravec, P. Kusnirak, and K. Hornoch, Ondrejov Observatory; Yu. Krugly and V. Chiorny, Institute of Astronomy, Kharkiv National University, National Academy of Science of Ukraine; M. Husarik and M. Pikler, Skalnate Pleso Observatory; J. Vilagi, S. Gajdos, and A. Galad, Modra Observatory; W. Cooney, J. Gross, and D. Terrell, Sonoita Research Observatory, Sonoita, AZ; N. Gaftonyuk, Simeiz Observatory; R. Stephens, Goat Mountain Astronomical Research Station, Yucca Valley, CA; R. Durkee, Minneapolis, MN; F. Marchis and M. Baek, SETI Institute; B. Macomber, University of California at Berkeley; V. Reddy, Department of Earth System Science and Policy, University of North Dakota, Grand Forks; F. Colas and J. Lecacheux, IMCCE and Pic du Midi Observatory; and J. Ries, McDonald Observatory, report that photometric observations obtained during Sept. 2- Nov. 9 reveal that minor planet (16635) is a binary system with an orbital period of 32.25 ± 0.03 hr. Additive rotation lightcurves of system's components have periods 2.2083 ± 0.0002 and 7.622 ± 0.002 hr and amplitudes 0.17 and 0.05 mag, respectively. Mutual events indicate a lower limit on the secondary-to-primary mean-diameter ratio of 0.27. Calibrated data give an estimated mean absolute magnitude H_R = 14.0 ± 0.3, assuming G = 0.15 ± 0.2. (C) Copyright 2007 CBAT 2007 November 19 (CBET 1143) Daniel W. E. Green (1453) FENNIA B. D. Warner, Palmer Divide Observatory, Colorado Springs, CO; A. W. Harris, Space Science Institute; P. Pravec, Ondrejov Observatory; R. D. Stephens, Goat Mountain Astronomical Research Station, Yucca Valley, CA; D. Pray, Carbuncle Hill Observatory, Greene, RI; W. Cooney, J. Gross, and D. Terrell, Sonoita Research Observatory, Sonoita, AZ; S. Gajdos and A. Galad, Modra Observatory; and Yu. Krugly, Institute of Astronomy of Kharkiv Science of Ukraine, report that photometric observations made during Nov. 4-23 reveal that minor planet (1453) is a binary system with an orbital period of 22.99 ± 0.01 hr. The primary shows a period of 4.4121 ± 0.0001 hr, and it has a lightcurve amplitude of 0.18 mag, suggesting a nearly spheroidal shape. Mutual eclipse/occultation events indicate a lower limit on the secondary-to-primary mean-diameter ratio of 0.28 ± 0.02. (C) Copyright 2007 CBAT 2007 December 1 (CBET 1150) Daniel W. E. Green 2005 NB_7 P. Kusnirak and P. Pravec, Ondrejov Observatory; A. Galad and L. Kornos, Modra Observatory; and W. Cooney, J. Gross, and D. Terrell, Sonoita Research Observatory, Sonoita, AZ, U.S.A., report that photometric observations obtained during Apr. 30-May 11 reveal the following information for the binary minor planet 2005 NB_7 (cf. IAUC 8936): orbital period = 15.28 ±0.01 hr (same as the secondary's rotation period); primary's rotation period = 3.4883 ± 0.0002 hr; primary's lightcurve amplitude = 0.13 mag, suggesting a nearly spheroidal shape; secondary's lightcurve amplitude = 0.09 mag; lower limit on the secondary-to-primary mean-diameter ratio = 0.32. (C) Copyright 2008 CBAT 2008 May 23 (CBET 1383) Daniel W. E. Green" [2008-05-26 13:29, Ondrejov] IAUC'S Circular No. 8630 Central Bureau for Astronomical Telegrams INTERNATIONAL ASTRONOMICAL UNION Mailstop 18, Smithsonian Astrophysical Observatory, Cambridge , MA 02138 , U.S.A. IAUSUBS@CFA.HARVARD.EDU or FAX 617-495-7231 (subscriptions) CBAT@CFA.HARVARD.EDU (science) URL http://cfa-www.harvard.edu/iau/cbat.html ISSN 0081-0304 Phone 617-495-7440/7244/7444 (for emergency use only) (2006) POLONSKAYA D. Pray, Greene , RI ; P. Pravec and P. Kusnirak, Ondrejov Observatory; and W. Cooney , J. Gross and D. Terrell, Sonoita Research Observatory, report that observations obtained during Nov.1-13 show that the minor planet (2006) consists of a pair of bodies orbiting each other with a period of 19.15 +/- 0.02 hr and producing mutual eclipse/occultation events 0.06-mag deep. There are present two rotational lightcurves with periods of 3.1183 +/-0.0002 and 6.656 +/- 0.001 hr, with amplitudes of 0.08 and 0.06 mag, respectively, that persist during the mutual events. This suggests that either the system is binary with both bodies rotating non- synchronously with the orbital motion or there is a third body producing the additional period. A lower limit on the mean- diameter ratio of the eclipsing pair is 0.22. Further observations are needed to fully resolve the system. (C) Copyright 2005 CBAT 2005 November 16 (8630) Daniel W. E. Green Circular No. 8609 Central Bureau for Astronomical Telegrams INTERNATIONAL ASTRONOMICAL UNION Mailstop 18, Smithsonian Astrophysical Observatory, Cambridge , MA 02138 , U.S.A. (3982) KASTEL P. Pravec and P. Kusnirak, Ondrejov Observatory; L. Kornos and J. Vilagi, Modra Observatory; D. Pray, Coventry, RI; R. Durkee, Minneapolis, MN; and W. Cooney, J. Gross and D. Terrell, Sonoita Research Observatory, AZ, report that photometric observations obtained during Sept. 24-29 reveal that (3982) has a lightcurve consisting of two linearly additive components with periods 8.488 and 5.835 (or possibly 2.918) hr and amplitudes 0.27 and 0.08 mag, respectively. No attenuations due to occultations/eclipses were seen, so the proposed interpretation of binary nature of the minor planet needs to be confirmed with further observations. (C) Copyright 2005 CBAT 2005 April 13 (8511) Daniel W. E. Green (4951) IWAMOTO V. Reddy, Department of Earth System Science and Policy, University of North Dakota, Grand Forks; R. Dyvig, Badlands Observatory, Quinn, SD; P. Pravec and P. Kusnirak, Ondrejov Observatory; A. Galad, L. Kornos, S. Gajdos, and J. Vilagi, Modra Observatory; D. Pray, Carbuncle Hill Observatory, Greene, RI; W.Cooney, J. Gross, and D. Terrell, Sonoita Research Observatory, Sonoita, AZ; Yu. Krugly, Kharkiv Observatory; J. Ries, McDonald Observatory; K. Archer, Ironwood Observatory, Oahu, HI; J. Oey, Leura, N.S.W., Australia; M. Pikler and M. Husarik, Skalnate Pleso Observatory; R. Durkee, Minneapolis, MN; F. Colas, Pic du Midi Observatory; and A. Harris, Space Science Institute, report that photometric observations obtained during 2006 Dec. 25.1 to 2007 Mar.23.9 UT reveal that minor planet (4951) is a synchronous binary system with a period of 118.0 ± 0.2 hours. A combined rotation lightcurve has an amplitude of 0.34 mag, and superimposed mutual events indicate a lower limit on a secondary-to-primary mean- diameter ratio of 0.76. An estimated mean absolute magnitude in the Cousins R system of 13.26 ± 0.05 and measured color index of V-R = +0.48 ± 0.03 give an absolute V magnitude of 13.74 ± 0.06. This yields estimated mean diameters for the two bodies of 4.0 and3.5 km (uncertain by about 20 percent), assuming a geometric V albedo of 0.20 ± 0.07 for its 'S' classification from 'SMASS II'visible spectroscopy. The system's parameters are extraordinary in comparison with other known small binaries, in terms of system angular momentum and evolution to its present synchronous state; thus, further observations are warranted. IBVS Publications GW Cancri: A W-type W UMa System with Complete Eclipses BVI_c light curves of GW Cnc and the fits from the Wilson-Devinney solution. Clickhere for complete IBVS publication 5625 Photometric Variability in the Strongly Interacting Binary DK Canum Venaticorum UBVR_cI_c light curves of DK CVn from 2002. R_c light curve of DK CVn in 2003 compared with the 2002 light curve. R_c light curve of DK CVn in 2004 compared with the 2003 light curve. R_c light curve of DK CVn showing variability on monthly timescales in 2005. DK CVn flare event on HJD 2453395. Clickhere for the complete IBVS publication 5642 Partial Eclipses in BR Cygni BVR_cI_c light curves of BR Cyg and the fits from the Wilson-Devinney solution. Clickhere for the complete IBVS publication 5646 The Absolute Dimensions of the Overcontact Binary FI Bootis Clickhere for the link to the Astronomical Journal article 132:1153-1157 2006, September The Classical Algol XZ UMa -- Observations and Analysis Clickhere for the complete IBVS publication 5715.