Randy Moenctu Web Site Editor WWW Page: Http:/ /Lamar.Colostate.Edu
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
AAS/AIAA Astrodynamics Specialist Conference
DRAFT version: 7/15/2011 11:04 AM http://www.alyeskaresort.com AAS/AIAA Astrodynamics Specialist Conference July 31 ‐ August 4, 2011 Girdwood, Alaska AAS General Chair AIAA General Chair Ryan P. Russell William Todd Cerven Georgia Institute of Technology The Aerospace Corporation AAS Technical Chair AIAA Technical Chair Hanspeter Schaub Brian C. Gunter University of Colorado Delft University of Technology DRAFT version: 7/15/2011 11:04 AM http://www.alyeskaresort.com Cover images: Top right: Conference Location: Aleyska Resort in Girdwood Alaska. Middle left: Cassini looking back at an eclipsed Saturn, Astronomy picture of the day 2006 Oct 16, credit CICLOPS, JPL, ESA, NASA; Middle right: Shuttle shadow in the sunset (in honor of the end of the Shuttle Era), Astronomy picture of the day 2010 February 16, credit: Expedition 22 Crew, NASA. Bottom right: Comet Hartley 2 Flyby, Astronomy picture of the day 2010 Nov 5, Credit: NASA, JPL-Caltech, UMD, EPOXI Mission DRAFT version: 7/15/2011 11:04 AM http://www.alyeskaresort.com Table of Contents Registration ............................................................................................................................................... 5 Schedule of Events ................................................................................................................................... 6 Conference Center Layout ........................................................................................................................ 7 Conference Location: The Hotel Alyeska ............................................................................................... -
The Minor Planet Bulletin
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 36, NUMBER 3, A.D. 2009 JULY-SEPTEMBER 77. PHOTOMETRIC MEASUREMENTS OF 343 OSTARA Our data can be obtained from http://www.uwec.edu/physics/ AND OTHER ASTEROIDS AT HOBBS OBSERVATORY asteroid/. Lyle Ford, George Stecher, Kayla Lorenzen, and Cole Cook Acknowledgements Department of Physics and Astronomy University of Wisconsin-Eau Claire We thank the Theodore Dunham Fund for Astrophysics, the Eau Claire, WI 54702-4004 National Science Foundation (award number 0519006), the [email protected] University of Wisconsin-Eau Claire Office of Research and Sponsored Programs, and the University of Wisconsin-Eau Claire (Received: 2009 Feb 11) Blugold Fellow and McNair programs for financial support. References We observed 343 Ostara on 2008 October 4 and obtained R and V standard magnitudes. The period was Binzel, R.P. (1987). “A Photoelectric Survey of 130 Asteroids”, found to be significantly greater than the previously Icarus 72, 135-208. reported value of 6.42 hours. Measurements of 2660 Wasserman and (17010) 1999 CQ72 made on 2008 Stecher, G.J., Ford, L.A., and Elbert, J.D. (1999). “Equipping a March 25 are also reported. 0.6 Meter Alt-Azimuth Telescope for Photometry”, IAPPP Comm, 76, 68-74. We made R band and V band photometric measurements of 343 Warner, B.D. (2006). A Practical Guide to Lightcurve Photometry Ostara on 2008 October 4 using the 0.6 m “Air Force” Telescope and Analysis. Springer, New York, NY. located at Hobbs Observatory (MPC code 750) near Fall Creek, Wisconsin. -
17 Minor Planet Bulletin 45 (2018) LIGHTCURVE and ROTATION
17 LIGHTCURVE AND ROTATION PERIOD DETERMINATION FOR 5813 EIZABURO AND (11745) 1999 NH3 Fabio Salvaggio Wild Boar Remote Observatory (K49) 21047 – Saronno (VA), ITALY [email protected] Massimo Banfi Wild Boar Remote Observatory (K49) Nova Milanese (MI), ITALY Alessandro Marchini Astronomical Observatory, DSFTA - University of Siena (K54) via Roma, 56, 53100 – Siena, ITALY Riccardo Papini Wild Boar Remote Observatory (K49) San Casciano in Val di Pesa (FI), ITALY (Received: 2017 Sep 20) Photometric observations of the main-belt asteroids 5813 Eizaburo and (11745) 1999 NH3 performed made in 2017 August revealed a bimodal lightcurve phased to 2.876 ± 0.002 h for 5813 Eizaburo and 3.280 ± 0.001 h for (11745) 1999 NH3 as the most likely synodic rotational periods for these asteroids. Lightcurve analysis for main-belt asteroids 5813 Eizaburo and (11745) 1999 NH3 was done using images obtained in 2017 August at the Astronomical Observatory of the University of (11745) 1999 NH3 is a main-belt asteroid discovered on 1999 July Siena (Italy) and at the Wild Boar Remote Observatory (K49). 13 by LINEAR at Socorro. The orbit has a semi-major axis of about 2.70 AU, eccentricity 0.179, and orbital period of about 4.56 At the Astronomical Observatory of the University of Siena, data years. We observed this asteroid from 2017 August 14-18. The were obtained with 0.30-m f/5.6 Maksutov-Cassegrain telescope, collaborative observations resulted in five sessions with a total of SBIG STL-6303E NABG CCD camera, and clear filter; the pixel 182 data points. The result is a bimodal lightcurve phased to 3.280 scale was 2.26 arcsec in binning 2x2. -
Aqueous Alteration on Main Belt Primitive Asteroids: Results from Visible Spectroscopy1
Aqueous alteration on main belt primitive asteroids: results from visible spectroscopy1 S. Fornasier1,2, C. Lantz1,2, M.A. Barucci1, M. Lazzarin3 1 LESIA, Observatoire de Paris, CNRS, UPMC Univ Paris 06, Univ. Paris Diderot, 5 Place J. Janssen, 92195 Meudon Pricipal Cedex, France 2 Univ. Paris Diderot, Sorbonne Paris Cit´e, 4 rue Elsa Morante, 75205 Paris Cedex 13 3 Department of Physics and Astronomy of the University of Padova, Via Marzolo 8 35131 Padova, Italy Submitted to Icarus: November 2013, accepted on 28 January 2014 e-mail: [email protected]; fax: +33145077144; phone: +33145077746 Manuscript pages: 38; Figures: 13 ; Tables: 5 Running head: Aqueous alteration on primitive asteroids Send correspondence to: Sonia Fornasier LESIA-Observatoire de Paris arXiv:1402.0175v1 [astro-ph.EP] 2 Feb 2014 Batiment 17 5, Place Jules Janssen 92195 Meudon Cedex France e-mail: [email protected] 1Based on observations carried out at the European Southern Observatory (ESO), La Silla, Chile, ESO proposals 062.S-0173 and 064.S-0205 (PI M. Lazzarin) Preprint submitted to Elsevier September 27, 2018 fax: +33145077144 phone: +33145077746 2 Aqueous alteration on main belt primitive asteroids: results from visible spectroscopy1 S. Fornasier1,2, C. Lantz1,2, M.A. Barucci1, M. Lazzarin3 Abstract This work focuses on the study of the aqueous alteration process which acted in the main belt and produced hydrated minerals on the altered asteroids. Hydrated minerals have been found mainly on Mars surface, on main belt primitive asteroids and possibly also on few TNOs. These materials have been produced by hydration of pristine anhydrous silicates during the aqueous alteration process, that, to be active, needed the presence of liquid water under low temperature conditions (below 320 K) to chemically alter the minerals. -
The Minor Planet Bulletin
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 35, NUMBER 3, A.D. 2008 JULY-SEPTEMBER 95. ASTEROID LIGHTCURVE ANALYSIS AT SCT/ST-9E, or 0.35m SCT/STL-1001E. Depending on the THE PALMER DIVIDE OBSERVATORY: binning used, the scale for the images ranged from 1.2-2.5 DECEMBER 2007 – MARCH 2008 arcseconds/pixel. Exposure times were 90–240 s. Most observations were made with no filter. On occasion, e.g., when a Brian D. Warner nearly full moon was present, an R filter was used to decrease the Palmer Divide Observatory/Space Science Institute sky background noise. Guiding was used in almost all cases. 17995 Bakers Farm Rd., Colorado Springs, CO 80908 [email protected] All images were measured using MPO Canopus, which employs differential aperture photometry to determine the values used for (Received: 6 March) analysis. Period analysis was also done using MPO Canopus, which incorporates the Fourier analysis algorithm developed by Harris (1989). Lightcurves for 17 asteroids were obtained at the Palmer Divide Observatory from December 2007 to early The results are summarized in the table below, as are individual March 2008: 793 Arizona, 1092 Lilium, 2093 plots. The data and curves are presented without comment except Genichesk, 3086 Kalbaugh, 4859 Fraknoi, 5806 when warranted. Column 3 gives the full range of dates of Archieroy, 6296 Cleveland, 6310 Jankonke, 6384 observations; column 4 gives the number of data points used in the Kervin, (7283) 1989 TX15, 7560 Spudis, (7579) 1990 analysis. Column 5 gives the range of phase angles. -
The Ch-‐Class Asteroids
The Ch-class asteroids: Connecting a visible taxonomic class to a 3-µm band shape Andrew S. Rivkin1*, Cristina A. Thomas2+, Ellen S. Howell3*^, Joshua P. Emery4* 1. The Johns Hopkins University Applied Physics Laboratory 2. NASA Goddard Space Flight Center, 3. Arecibo Observatory, USRA 4. University of Tennessee Accepted to The Astronomical Journal 3 November 2015 *Visiting Astronomer at the Infrared Telescope Facility, which is operated by the University of Hawaii under Cooperative Agreement no. NNX-08AE38A with the National Aeronautics and Space Administration, Science Mission Directorate, Planetary Astronomy Program. +Currently also at the Planetary Science Institute. Work done while supported by an appointment to the NASA Postdoctoral Program, administered by Oak Ridge Associated Universities through a contract with NASA. ^Currently at Lunar and Planetary Laboratory, University of Arizona, Tucson AZ Abstract Asteroids belonging to the Ch spectral taxonomic class are defined by the presence of an absorption near 0.7 μm, which is interpreted as due to Fe-bearing phyllosilicates. Phyllosilicates also cause strong absorptions in the 3-μm region, as do other hydrated and hydroxylated minerals and H2O ice. Over the past decade, spectral observations have revealed different 3-µm band shapes the asteroid population. Although a formal taxonomy is yet to be fully established, the “Pallas-type” spectral group is most consistent with the presence of phyllosilicates. If Ch class and Pallas type are both indicative of phyllosilicates, then all Ch-class asteroids should also be Pallas-type. In order to test this hypothesis, we obtained 42 observations of 36 Ch-class asteroids in the 2- to 4-µm spectral region. -
Cumulative Index to Volumes 1-45
The Minor Planet Bulletin Cumulative Index 1 Table of Contents Tedesco, E. F. “Determination of the Index to Volume 1 (1974) Absolute Magnitude and Phase Index to Volume 1 (1974) ..................... 1 Coefficient of Minor Planet 887 Alinda” Index to Volume 2 (1975) ..................... 1 Chapman, C. R. “The Impossibility of 25-27. Index to Volume 3 (1976) ..................... 1 Observing Asteroid Surfaces” 17. Index to Volume 4 (1977) ..................... 2 Tedesco, E. F. “On the Brightnesses of Index to Volume 5 (1978) ..................... 2 Dunham, D. W. (Letter regarding 1 Ceres Asteroids” 3-9. Index to Volume 6 (1979) ..................... 3 occultation) 35. Index to Volume 7 (1980) ..................... 3 Wallentine, D. and Porter, A. Index to Volume 8 (1981) ..................... 3 Hodgson, R. G. “Useful Work on Minor “Opportunities for Visual Photometry of Index to Volume 9 (1982) ..................... 4 Planets” 1-4. Selected Minor Planets, April - June Index to Volume 10 (1983) ................... 4 1975” 31-33. Index to Volume 11 (1984) ................... 4 Hodgson, R. G. “Implications of Recent Index to Volume 12 (1985) ................... 4 Diameter and Mass Determinations of Welch, D., Binzel, R., and Patterson, J. Comprehensive Index to Volumes 1-12 5 Ceres” 24-28. “The Rotation Period of 18 Melpomene” Index to Volume 13 (1986) ................... 5 20-21. Hodgson, R. G. “Minor Planet Work for Index to Volume 14 (1987) ................... 5 Smaller Observatories” 30-35. Index to Volume 15 (1988) ................... 6 Index to Volume 3 (1976) Index to Volume 16 (1989) ................... 6 Hodgson, R. G. “Observations of 887 Index to Volume 17 (1990) ................... 6 Alinda” 36-37. Chapman, C. R. “Close Approach Index to Volume 18 (1991) .................. -
The Minor Planet Bulletin 40 (2013) 125 CS3 Observations on Jan 13 and 14 Were Made with a 0.35-M Schmidt-Cassegrain and SBIG ST-9XE
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 40, NUMBER 3, A.D. 2013 JULY-SEPTEMBER 119. SOMETHING OLD, SOMETHINGS NEW: figure shows the lightcurve after removing the rotation of the THREE BINARY DISCOVERIES primary, thus revealing the mutual events and other features due to FROM THE PALMER DIVIDE OBSERVATORY the satellite. The latter often includes an upward bowing between the events, indicating an elongated satellite that is tidally-locked to Brian D. Warner its orbital period. Palmer Divide Observatory 17995 Bakers Farm Rd., Colorado Springs, CO 80908 4383 Suruga. Observations of 4383 Suruga were made from 2013 [email protected] Feb 2-13. Initial observations were made with a 0.35-m Schmidt- Cassegrain and Finger Lakes FLI-1001E CCD camera. When (Received: 10 March) indications of a satellite were seen in those first data sets, the target was moved to a 0.5-m Ritchey-Chretien with FLI-1001E to improve the signal-to-noise ratio. Data on the order of 0.01-0.02 Analysis of new CCD photometric observations in early mag are usually required for reliable detections of mutual events 2013 of the Vestoid asteroid 4383 Suruga and Hungaria (occultations and/or eclipses) caused by a satellite. asteroid (53432) 1999 UT55 showed that the two are binary systems. A review of data from 2005 for the The results of the analysis are shown in Figures 1-3. The period of Hungaria asteroid 4440 Tchantches indicates that the the primary is 3.4068 ± 0.0003 h with an amplitude of 0.14 ± 0.01 original analysis probably overlooked a satellite. -
89 Minor Planet Bulletin 47 (2020) LIGHTCURVE PHOTOMETRY
89 LIGHTCURVE PHOTOMETRY OPPORTUNITIES: The SR magnitudes should be used when observing without (or 2021 JANUARY-MARCH with a Clear) filter and typical CCD cameras (e.g., FLI, SBIG, etc.) with a KAF-E chip (blue enhanced) or another chip with Brian D. Warner similar response. This is because those chips have a very good Center for Solar System Studies / MoreData! linear fit of catalog versus instrumental magnitude for the Rc and 446 Sycamore Ave. SR bands and so, if using near-solar color stars, there is no need Eaton, CO 80615 USA for additional reductions such as color term correction. [email protected] Regarding H-G observations, the question of how much data is Alan W. Harris enough is often raised. The answer is, “It depends on the nature of MoreData! the observing project.” To that, we’d add that having just a few La Cañada, CA 91011-3364 USA data points at each observing run places a much greater demand on having accurate magnitudes. If those requirements are on the order Josef Ďurech of 0.02 mag, that stretches the limits even when using the high- Astronomical Institute quality catalogs. Charles University 18000 Prague, CZECH REPUBLIC The H-G system is based on average light at the time of the [email protected] observations, i.e., the amplitude of the lightcurve at the time must be known and, if necessary, those few data points be corrected so Lance A.M. Benner that they correspond to “mid-light” at the time. Since the Jet Propulsion Laboratory amplitude often changes as the asteroid recedes or approaches, it’s Pasadena, CA 91109-8099 USA necessary to obtain enough data points during each observing run [email protected] to establish or reasonably predict the mid-light magnitude. -
Lightcurve Based Determination of 10 Hygiea's Rotational Period with Trappist-North
1 LIGHTCURVE BASED DETERMINATION OF 199.C-0074 (Vernazza et al., 2018) aiming to determine precise 10 HYGIEA’S ROTATIONAL PERIOD volumes and densities of the 40 largest MBAs, we started WITH TRAPPIST-NORTH AND -SOUTH extensive photometric observations of Hygiea to refine its rotation period and help in the shape and spin axis determination. Such a Marin Ferrais1,2, Emmanuël Jehin1, Pierre Vernazza2, long period is challenging to cover, especially when it is close to Laurent Jorda2, Youssef Moulane1, Francisco J. Pozuelos1, 24 h (the 27.6 h period translates in a phase shift of only 13% of 1 1,3 3 Jean Manfroid , Khalid Barkaoui , Zouhair Benkhaldoun the rotation each night), explaining the lack of dense lightcurves for this large and bright asteroid. To tackle this challenge, the 1 Space sciences, Technologies & complementarity of the two TRAPPIST telescopes at two different Astrophysics Research (STAR) Institute longitudes was decisive to acquire long and continuous University of Liège photometric series as illustrated in Ferrais et al. (2020). Allée du 6 Août 19, 4000 Liège, BELGIUM [email protected] We observed Hygiea in 2018 from September 10 to October 17 with TN and TS using the Johnson-Cousins broad band Rc filter, 2 Aix Marseille Université, CNRS, LAM, Laboratoire no binning, and an exposure time of 8 seconds. As more data were d'Astrophysique de Marseille, Marseille, FRANCE gathered, the phased lightcurve started to show a classic double- 3 sinusoidal shape with the previously reported period but with the Oukaïmenden Observatory high quality of the data, we noticed it was perfectly symmetric Cadi Ayyad University, Marrakech, MOROCCO (see Fig.