DOCSLIB.ORG

Transiti Pianeti Extrasolari Visibili Dall'italia (Long. 9 E Lat 44 N)

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Transiti Pianeti Extrasolari Visibili Dall'italia (Long. 9 E Lat 44 N) programma di Claudio Lopresti Transiti pianeti extrasolari visibili dall'Italia (long. 9 E lat 44 N) base dati: fonte NASA) PlanetName depth period duration Ingress (date) Ingress (U.T.) Center (U.T.) Egress (U.T.) 2.11 4.06 0.1168 00:34 02:03 03:32 WASP-39 b lunedì 5 maggio 2014 38.22 209.91 27.54 233.3 13.32 251.7 R.A. DEC. magV. 14h29m18.41s -03d26m40.3s 12.11 0 alt az alt az alt az 2.525 3.09 0.0928 00:35 01:53 03:11 WASP-10 b lunedì 5 maggio 2014 9.82 55.3 22.12 67 35.52 78.34 R.A. DEC. magV. 23h15m58.30s +31d27m46.3s 12.7 0 alt az alt az alt az 7.20 0.124 01:21 02:59 04:38 Kepler-49 b lunedì 5 maggio 2014 60.39 82.45 78.08 101.3 82.37 246.7 R.A. DEC. magV. 19h29m10.70s +40d35m30.5s 15.5 0 alt az alt az alt az 1.35 0.0862 18:30 19:33 20:36 HATS-2 b lunedì 5 maggio 2014 19.14 154.14 22.72 169.3 23.27 185.2 R.A. DEC. magV. 11h46m57.38s -22d33m46.8s 13.562 0 alt az alt az alt az 0.0344 45.29 0.286 19:10 23:16 03:23 Kepler-10 c lunedì 5 maggio 2014 15.48 32.71 47.55 58.15 83.62 11.1 R.A. DEC. magV. 19h02m43.05s +50d14m28.7s 10.96 0 alt az alt az alt az HD 149026 b HD 149026 0.2933 2.88 0.135 19:31 21:12 22:52 HIP 80838 lunedì 5 maggio 2014 30.6 64.47 47.65 77.24 65.6 92.35 R.A. DEC. magV. 16h30m29.62s +38d20m50.3s 8.15 0 alt az alt az alt az 1.17 3.92 0.143 19:32 21:50 00:09 HAT-P-9 b lunedì 5 maggio 2014 48 280.48 24.64 298.7 5.25 319 R.A. DEC. magV. 07h20m40.45s +37d08m26.3s 0 alt az alt az alt az 2.92 0.1345 19:49 21:36 23:23 HAT-P-13 b lunedì 5 maggio 2014 62.13 291.17 44.57 299 28.58 309.7 R.A. DEC. magV. 08h39m31.81s +47d21m07.4s 10.62 0 alt az alt az alt az 1.008 2.34 0.1118 21:11 22:34 23:57 WASP-24 b lunedì 5 maggio 2014 37.28 131.58 46.05 156.9 48.11 187.4 R.A. DEC. magV. 15h08m51.74s +02d20m35.9s 11.3 0 alt az alt az alt az 0.65 5.01 0.2141 21:34 01:20 05:06 HAT-P-31 b lunedì 5 maggio 2014 28.17 79.36 66.85 133.2 54.74 252.9 R.A. DEC. magV. 18h06m09.05s +26d25m36.0s 11.66 0 alt az alt az alt az 1.019 4.62 0.1484 22:07 23:57 01:46 WASP-56 b lunedì 5 maggio 2014 62.75 226.67 45.15 258.5 25.48 278.2 R.A. DEC. magV. 12h13m27.91s +23d03m20.5s 0 alt az alt az alt az 1.873 3.03 0.104 22:34 23:50 01:05 TrES-1 b lunedì 5 maggio 2014 34.6 70.03 47.69 80.14 61.21 92 R.A. DEC. magV. 19h04m09.84s +36d37m57.5s 0 alt az alt az alt az 1.899 2.80 0.0971 22:41 23:55 01:10 HAT-P-37 b lunedì 5 maggio 2014 43.36 54.58 54.63 59.13 66.26 60.13 R.A. DEC. magV. 18h57m11.05s +51d16m08.9s 13.23 0 alt az alt az alt az 1.1449 2.99 0.1042 23:30 00:57 02:24 CoRoT-11 b lunedì 5 maggio 2014 28.61 111.29 41.95 132.4 50.58 161.5 R.A. DEC. magV. 18h42m44.94s +05d56m15.7s 12.94 0 alt az alt az alt az 5.51 0.1131 00:28 01:53 03:18 HAT-P-18 b martedì 6 maggio 2014 75.05 227.1 61.23 259.3 45.96 275.2 R.A. DEC. magV. 17h05m23.15s +33d00m45.0s 12.76 0 alt az alt az alt az 5.91 0.1154 18:58 20:21 21:44 Kepler-28 b martedì 6 maggio 2014 19.61 49.34 31.81 59.69 45.31 69.06 R.A. DEC. magV. 19h28m32.89s +42d25m45.9s 15.5 0 alt az alt az alt az 1.026 1.85 0.114 19:32 20:58 22:24 WASP-3 b martedì 6 maggio 2014 28.85 66.84 43.6 78.49 58.99 91.91 R.A. DEC. magV. 18h34m31.63s +35d39m41.5s 10.64 0 alt az alt az alt az 10.91 0.1191 19:45 21:30 23:16 Kepler-49 c martedì 6 maggio 2014 25.15 56.92 42.12 69.74 60.52 82.55 R.A. DEC. magV. 19h29m10.70s +40d35m30.5s 15.5 0 alt az alt az alt az 8.15 0.1675 19:45 21:45 23:46 Kepler-24 b martedì 6 maggio 2014 24.91 59.84 44.95 75.25 66.48 93.31 R.A. DEC. magV. 19h21m39.18s +38d20m37.5s 15.5 0 alt az alt az alt az 1.45 5.02 0.1582 22:23 00:24 02:24 WASP-58 b martedì 6 maggio 2014 64.93 74.78 86.09 70.72 72.25 282.6 R.A. DEC. magV. 18h18m48.25s +45d10m19.3s 11.66 0 alt az alt az alt az 2.71 1.75 0.0754 00:15 01:11 02:06 WASP-52 b mercoledì 7 maggio 2014 32.47 111.31 41.3 124.5 48.66 141 R.A. DEC. magV. 23h13m58.74s +08d45m40.5s 12 0 alt az alt az alt az 0.86 3.69 0.1863 18:32 20:49 23:07 WASP-54 b mercoledì 7 maggio 2014 45.61 187.77 33.44 230.1 11.22 258.8 R.A. DEC. magV. 13h41m49.04s -00d07m41.1s 0 alt az alt az alt az 4.78 0.1184 19:11 20:45 22:20 Kepler-48 b mercoledì 7 maggio 2014 34.23 63.58 50.15 74.64 66.95 86.71 R.A. DEC. magV. 19h56m33.41s +40d56m56.5s 13.5 0 alt az alt az alt az 2.525 3.09 0.0928 21:06 22:25 23:43 WASP-10 b mercoledì 7 maggio 2014 15.17 60.66 28.09 72.12 41.87 83.75 R.A. DEC. magV. 23h15m58.30s +31d27m46.3s 12.7 0 alt az alt az alt az 0.8255 3.85 0.1461 22:11 00:02 01:53 HAT-P-6 b mercoledì 7 maggio 2014 28.57 57.12 46.43 69.72 65.76 81.88 R.A. DEC. magV. 23h39m05.82s +42d27m57.5s 10.5 0 alt az alt az alt az HAT-P-11 b 4.89 0.0957 23:01 00:16 01:30 HIP 97657 mercoledì 7 maggio 2014 76 66.26 85.88 7.36 77.04 294.6 R.A. DEC. magV. 19h50m50.24s +48d04m51.1s 9.59 0 alt az alt az alt az 210.61 0.5247 17:33 23:58 06:24 KOI-351 g giovedì 8 maggio 2014 50.87 61.11 63.21 295.2 11.13 332.2 R.A. DEC. magV. 18h57m44.04s +49d18m18.6s 0 alt az alt az alt az 0.8255 3.85 0.1461 17:58 19:49 21:39 HAT-P-6 b giovedì 8 maggio 2014 10.8 39.54 25.45 54.56 42.93 67.45 R.A. DEC. magV. 23h39m05.82s +42d27m57.5s 10.5 0 alt az alt az alt az 0.0282 5.86 0.1637 19:08 21:08 23:08 Kepler-65 c giovedì 8 maggio 2014 61.94 82.35 83.3 112.3 73.77 267.5 R.A. DEC. magV. 19h14m45.29s +41d09m04.2s 11.6 0 alt az alt az alt az 1.0536 1.21 0.0908 19:20 20:31 21:41 HAT-P-23 b giovedì 8 maggio 2014 38.21 104.47 49.89 121.6 59.09 146.3 R.A. DEC. magV. 20h24m29.72s +16d45m43.7s 11.94 0 alt az alt az alt az 2.525 3.09 0.0928 19:22 20:41 21:59 WASP-10 b giovedì 8 maggio 2014 17.95 63.27 31.14 74.67 45.07 86.6 R.A. DEC. magV. 23h15m58.30s +31d27m46.3s 12.7 0 alt az alt az alt az HD 149026 b HD 149026 0.2933 2.88 0.135 20:12 21:53 23:33 HIP 80838 giovedì 8 maggio 2014 74.74 254.77 56.75 275.8 39.11 289.1 R.A. DEC. magV. 16h30m29.62s +38d20m50.3s 8.15 0 alt az alt az alt az 1.742 3.94 0.1238 20:18 21:50 23:22 XO-1 b giovedì 8 maggio 2014 62.99 243.3 47.07 265.7 30.62 281.0 R.A. DEC. magV. 16h02m11.84s +28d10m10.4s 11.3 0 alt az alt az alt az 0.82 3.19 0.1245 20:36 22:13 23:51 XO-3 b giovedì 8 maggio 2014 14.27 14.43 20.42 26.36 29.6 36.43 R.A.
Load more

Recommended publications
  • Catalog of Nearby Exoplanets
    Catalog of Nearby Exoplanets1 R. P. Butler2, J. T. Wright3, G. W. Marcy3,4, D. A Fischer3,4, S. S. Vogt5, C. G. Tinney6, H. R. A. Jones7, B. D. Carter8, J. A. Johnson3, C. McCarthy2,4, A. J. Penny9,10 ABSTRACT We present a catalog of nearby exoplanets. It contains the 172 known low- mass companions with orbits established through radial velocity and transit mea- surements around stars within 200 pc. We include 5 previously unpublished exo- planets orbiting the stars HD 11964, HD 66428, HD 99109, HD 107148, and HD 164922. We update orbits for 90 additional exoplanets including many whose orbits have not been revised since their announcement, and include radial ve- locity time series from the Lick, Keck, and Anglo-Australian Observatory planet searches. Both these new and previously published velocities are more precise here due to improvements in our data reduction pipeline, which we applied to archival spectra. We present a brief summary of the global properties of the known exoplanets, including their distributions of orbital semimajor axis, mini- mum mass, and orbital eccentricity. Subject headings: catalogs — stars: exoplanets — techniques: radial velocities 1Based on observations obtained at the W. M. Keck Observatory, which is operated jointly by the Uni- versity of California and the California Institute of Technology. The Keck Observatory was made possible by the generous financial support of the W. M. Keck Foundation. arXiv:astro-ph/0607493v1 21 Jul 2006 2Department of Terrestrial Magnetism, Carnegie Institute of Washington, 5241 Broad Branch Road NW, Washington, DC 20015-1305 3Department of Astronomy, 601 Campbell Hall, University of California, Berkeley, CA 94720-3411 4Department of Physics and Astronomy, San Francisco State University, San Francisco, CA 94132 5UCO/Lick Observatory, University of California, Santa Cruz, CA 95064 6Anglo-Australian Observatory, PO Box 296, Epping.
    [Show full text]
  • Naming the Extrasolar Planets
    Naming the extrasolar planets W. Lyra Max Planck Institute for Astronomy, K¨onigstuhl 17, 69177, Heidelberg, Germany [email protected] Abstract and OGLE-TR-182 b, which does not help educators convey the message that these planets are quite similar to Jupiter. Extrasolar planets are not named and are referred to only In stark contrast, the sentence“planet Apollo is a gas giant by their assigned scientific designation. The reason given like Jupiter” is heavily - yet invisibly - coated with Coper- by the IAU to not name the planets is that it is consid- nicanism. ered impractical as planets are expected to be common. I One reason given by the IAU for not considering naming advance some reasons as to why this logic is flawed, and sug- the extrasolar planets is that it is a task deemed impractical. gest names for the 403 extrasolar planet candidates known One source is quoted as having said “if planets are found to as of Oct 2009. The names follow a scheme of association occur very frequently in the Universe, a system of individual with the constellation that the host star pertains to, and names for planets might well rapidly be found equally im- therefore are mostly drawn from Roman-Greek mythology. practicable as it is for stars, as planet discoveries progress.” Other mythologies may also be used given that a suitable 1. This leads to a second argument. It is indeed impractical association is established. to name all stars. But some stars are named nonetheless. In fact, all other classes of astronomical bodies are named.
    [Show full text]
  • Arxiv:0809.1275V2
    How eccentric orbital solutions can hide planetary systems in 2:1 resonant orbits Guillem Anglada-Escud´e1, Mercedes L´opez-Morales1,2, John E. Chambers1 [email protected], [email protected], [email protected] ABSTRACT The Doppler technique measures the reflex radial motion of a star induced by the presence of companions and is the most successful method to detect ex- oplanets. If several planets are present, their signals will appear combined in the radial motion of the star, leading to potential misinterpretations of the data. Specifically, two planets in 2:1 resonant orbits can mimic the signal of a sin- gle planet in an eccentric orbit. We quantify the implications of this statistical degeneracy for a representative sample of the reported single exoplanets with available datasets, finding that 1) around 35% percent of the published eccentric one-planet solutions are statistically indistinguishible from planetary systems in 2:1 orbital resonance, 2) another 40% cannot be statistically distinguished from a circular orbital solution and 3) planets with masses comparable to Earth could be hidden in known orbital solutions of eccentric super-Earths and Neptune mass planets. Subject headings: Exoplanets – Orbital dynamics – Planet detection – Doppler method arXiv:0809.1275v2 [astro-ph] 25 Nov 2009 Introduction Most of the +300 exoplanets found to date have been discovered using the Doppler tech- nique, which measures the reflex motion of the host star induced by the planets (Mayor & Queloz 1995; Marcy & Butler 1996). The diverse characteristics of these exoplanets are somewhat surprising. Many of them are similar in mass to Jupiter, but orbit much closer to their 1Carnegie Institution of Washington, Department of Terrestrial Magnetism, 5241 Broad Branch Rd.
    [Show full text]
  • Discovering the Growth Histories of Exoplanets: the Saturn Analog HD 149026B
    Discovering the Growth Histories of Exoplanets: The Saturn Analog HD 149026b Short title: The growth of HD 149026b Sarah E. Dodson-Robinson1 NASA Exoplanet Science Institute, California Institute of Technology 770 S. Wilson Ave, Pasadena, CA 91125 [email protected] Peter Bodenheimer UCO/Lick Observatory, University of California at Santa Cruz 1156 High St., Santa Cruz, CA 95064 1 Formerly Sarah E. Robinson ABSTRACT The transiting “hot Saturn” HD 149026b, which has the highest mean density of any confirmed planet in the Neptune-Jupiter mass range, has challenged theories of planet formation since its discovery in 2005. Previous investigations could not explain the origin of the planet’s 45-110 Earth-mass solid core without invoking catastrophes such as gas giant collisions or heavy planetesimal bombardment launched by neighboring planets. Here we show that HD 149026b’s large core can be successfully explained by the standard core accretion theory of planet formation. The keys to our reconstruction of HD 149026b are (1) applying a model of the solar nebula to describe the protoplanet nursery; (2) placing the planet initially on a long-period orbit at Saturn’s heliocentric distance of 9.5 AU; and (3) adjusting the solid mass in the HD 149026 disk to twice that of the solar nebula in accordance with the star’s heavy element enrichment. We show that the planet’s migration into its current orbit at 0.042 AU is consistent with our formation model. Our study of HD 149026b demonstrates that it is possible to discover the growth history of any planet with a well-defined core mass that orbits a solar-type star.
    [Show full text]
  • SILICON and OXYGEN ABUNDANCES in PLANET-HOST STARS Erik Brugamyer, Sarah E
    The Astrophysical Journal, 738:97 (11pp), 2011 September 1 doi:10.1088/0004-637X/738/1/97 C 2011. The American Astronomical Society. All rights reserved. Printed in the U.S.A. SILICON AND OXYGEN ABUNDANCES IN PLANET-HOST STARS Erik Brugamyer, Sarah E. Dodson-Robinson, William D. Cochran, and Christopher Sneden Department of Astronomy and McDonald Observatory, University of Texas at Austin, 1 University Station C1400, Austin, TX 78712, USA; [email protected] Received 2011 February 4; accepted 2011 June 22; published 2011 August 16 ABSTRACT The positive correlation between planet detection rate and host star iron abundance lends strong support to the core accretion theory of planet formation. However, iron is not the most significant mass contributor to the cores of giant planets. Since giant planet cores are thought to grow from silicate grains with icy mantles, the likelihood of gas giant formation should depend heavily on the oxygen and silicon abundance of the planet formation environment. Here we compare the silicon and oxygen abundances of a set of 76 planet hosts and a control sample of 80 metal-rich stars without any known giant planets. Our new, independent analysis was conducted using high resolution, high signal-to-noise data obtained at McDonald Observatory. Because we do not wish to simply reproduce the known planet–metallicity correlation, we have devised a statistical method for matching the underlying [Fe/H] distributions of our two sets of stars. We find a 99% probability that planet detection rate depends on the silicon abundance of the host star, over and above the observed planet–metallicity correlation.
    [Show full text]
  • When Extrasolar Planets Transit Their Parent Stars 701
    Charbonneau et al.: When Extrasolar Planets Transit Their Parent Stars 701 When Extrasolar Planets Transit Their Parent Stars David Charbonneau Harvard-Smithsonian Center for Astrophysics Timothy M. Brown High Altitude Observatory Adam Burrows University of Arizona Greg Laughlin University of California, Santa Cruz When extrasolar planets are observed to transit their parent stars, we are granted unprece- dented access to their physical properties. It is only for transiting planets that we are permitted direct estimates of the planetary masses and radii, which provide the fundamental constraints on models of their physical structure. In particular, precise determination of the radius may indicate the presence (or absence) of a core of solid material, which in turn would speak to the canonical formation model of gas accretion onto a core of ice and rock embedded in a proto- planetary disk. Furthermore, the radii of planets in close proximity to their stars are affected by tidal effects and the intense stellar radiation. As a result, some of these “hot Jupiters” are significantly larger than Jupiter in radius. Precision follow-up studies of such objects (notably with the spacebased platforms of the Hubble and Spitzer Space Telescopes) have enabled direct observation of their transmission spectra and emitted radiation. These data provide the first observational constraints on atmospheric models of these extrasolar gas giants, and permit a direct comparison with the gas giants of the solar system. Despite significant observational challenges, numerous transit surveys and quick-look radial velocity surveys are active, and promise to deliver an ever-increasing number of these precious objects. The detection of tran- sits of short-period Neptune-sized objects, whose existence was recently uncovered by the radial- velocity surveys, is eagerly anticipated.
    [Show full text]
  • Exoplanet Detection Techniques
    Exoplanet Detection Techniques Debra A. Fischer1, Andrew W. Howard2, Greg P. Laughlin3, Bruce Macintosh4, Suvrath Mahadevan5;6, Johannes Sahlmann7, Jennifer C. Yee8 We are still in the early days of exoplanet discovery. Astronomers are beginning to model the atmospheres and interiors of exoplanets and have developed a deeper understanding of processes of planet formation and evolution. However, we have yet to map out the full complexity of multi-planet architectures or to detect Earth analogues around nearby stars. Reaching these ambitious goals will require further improvements in instru- mentation and new analysis tools. In this chapter, we provide an overview of five observational techniques that are currently employed in the detection of exoplanets: optical and IR Doppler measurements, transit pho- tometry, direct imaging, microlensing, and astrometry. We provide a basic description of how each of these techniques works and discuss forefront developments that will result in new discoveries. We also highlight the observational limitations and synergies of each method and their connections to future space missions. Subject headings: 1. Introduction tary; in practice, they are not generally applied to the same sample of stars, so our detection of exoplanet architectures Humans have long wondered whether other solar sys- has been piecemeal. The explored parameter space of ex- tems exist around the billions of stars in our galaxy. In the oplanet systems is a patchwork quilt that still has several past two decades, we have progressed from a sample of one missing squares. to a collection of hundreds of exoplanetary systems. Instead of an orderly solar nebula model, we now realize that chaos 2.
    [Show full text]
  • Density Estimation for Projected Exoplanet Quantities
    Density Estimation for Projected Exoplanet Quantities Robert A. Brown Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 [email protected] ABSTRACT Exoplanet searches using radial velocity (RV) and microlensing (ML) produce samples of “projected” mass and orbital radius, respectively. We present a new method for estimating the probability density distribution (density) of the un- projected quantity from such samples. For a sample of n data values, the method involves solving n simultaneous linear equations to determine the weights of delta functions for the raw, unsmoothed density of the unprojected quantity that cause the associated cumulative distribution function (CDF) of the projected quantity to exactly reproduce the empirical CDF of the sample at the locations of the n data values. We smooth the raw density using nonparametric kernel density estimation with a normal kernel of bandwidth σ. We calibrate the dependence of σ on n by Monte Carlo experiments performed on samples drawn from a the- oretical density, in which the integrated square error is minimized. We scale this calibration to the ranges of real RV samples using the Normal Reference Rule. The resolution and amplitude accuracy of the estimated density improve with n. For typical RV and ML samples, we expect the fractional noise at the PDF peak to be approximately 80 n− log 2. For illustrations, we apply the new method to 67 RV values given a similar treatment by Jorissen et al. in 2001, and to the 308 RV values listed at exoplanets.org on 20 October 2010. In addition to an- alyzing observational results, our methods can be used to develop measurement arXiv:1011.3991v3 [astro-ph.IM] 21 Mar 2011 requirements—particularly on the minimum sample size n—for future programs, such as the microlensing survey of Earth-like exoplanets recommended by the Astro 2010 committee.
    [Show full text]
  • Orders of Magnitude (Length) - Wikipedia
    03/08/2018 Orders of magnitude (length) - Wikipedia Orders of magnitude (length) The following are examples of orders of magnitude for different lengths. Contents Overview Detailed list Subatomic Atomic to cellular Cellular to human scale Human to astronomical scale Astronomical less than 10 yoctometres 10 yoctometres 100 yoctometres 1 zeptometre 10 zeptometres 100 zeptometres 1 attometre 10 attometres 100 attometres 1 femtometre 10 femtometres 100 femtometres 1 picometre 10 picometres 100 picometres 1 nanometre 10 nanometres 100 nanometres 1 micrometre 10 micrometres 100 micrometres 1 millimetre 1 centimetre 1 decimetre Conversions Wavelengths Human-defined scales and structures Nature Astronomical 1 metre Conversions https://en.wikipedia.org/wiki/Orders_of_magnitude_(length) 1/44 03/08/2018 Orders of magnitude (length) - Wikipedia Human-defined scales and structures Sports Nature Astronomical 1 decametre Conversions Human-defined scales and structures Sports Nature Astronomical 1 hectometre Conversions Human-defined scales and structures Sports Nature Astronomical 1 kilometre Conversions Human-defined scales and structures Geographical Astronomical 10 kilometres Conversions Sports Human-defined scales and structures Geographical Astronomical 100 kilometres Conversions Human-defined scales and structures Geographical Astronomical 1 megametre Conversions Human-defined scales and structures Sports Geographical Astronomical 10 megametres Conversions Human-defined scales and structures Geographical Astronomical 100 megametres 1 gigametre
    [Show full text]
  • 1949 Celebrating 65 Years of Bringing Astronomy to North Texas 2014
    1949 Celebrating 65 Years of Bringing Astronomy to North Texas 2014 Contact information: Inside this issue: Info Officer (General Info)– [email protected]@fortworthastro.com Website Administrator – [email protected] Postal Address: Page Fort Worth Astronomical Society July Club Calendar 3 3812 Fenton Avenue Fort Worth, TX 76133 Celestial Events 4 Web Site: http://www.fortworthastro.org Facebook: http://tinyurl.com/3eutb22 Sky Chart 5 Twitter: http://twitter.com/ftwastro Yahoo! eGroup (members only): http://tinyurl.com/7qu5vkn Moon Phase Calendar 6 Officers (2014-2015): Mecury/Venus Data Sheet 7 President – Bruce Cowles, [email protected] Vice President – Russ Boatwright, [email protected] Young Astronomer News 8 Sec/Tres – Michelle Theisen, [email protected] Board Members: Cloudy Night Library 9 2014-2016 The Astrolabe 10 Mike Langohr Tree Oppermann AL Obs Club of the Month 14 2013-2015 Bill Nichols Constellation of the Month 15 Jim Craft Constellation Mythology 19 Cover Photo This is an HaLRGB image of M8 & Prior Club Meeting Minutes 23 M20, composed entirely from a T3i General Club Information 24 stack of one shot color. Collected the data over a period of two nights. That’s A Fact 24 Taken by FWAS member Jerry Keith November’s Full Moon 24 Observing Site Reminders: Be careful with fire, mind all local burn bans! FWAS Foto Files 25 Dark Site Usage Requirements (ALL MEMBERS): Maintain Dark-Sky Etiquettehttp://tinyurl.com/75hjajy ( ) Turn out your headlights at the gate! Sign
    [Show full text]
  • How to Size an Exoplanet? a Model Approach for Visualization Akos Kereszturi* Research Center for Astronomy and Earth Sciences, Hungary
    obiolog str y & f A O u o l t a r Kereszturi, Astrobiol Outreach 2013, 1:1 e n a r c u h o J Journal of Astrobiology & Outreach DOI: 10.4172/2332-2519.1000101 ISSN: 2332-2519 Research Article Article OpenOpen Access Access How to Size an Exoplanet? A Model Approach for Visualization Akos Kereszturi* Research Center for Astronomy and Earth Sciences, Hungary Abstract The realization and experiences with a physical exoplanet model in the education and outreach are described. During the tests with students in the classroom and adults at public demonstrations, the following conclusions were drawn: in the visualization it is effective to connect and install together the models of planets inside and outside the Solar System, where hot Jupiter’s easily fit into the orbit of Mercury. The size of planets and orbital distance could be more effectively visualized with this method, using the Solar System as a context. The exoplanet model helps to expand the imagination of the audience on how does a planetary system look like, what is getting important as diverse views of explanatory systems emerging in recent years. This inexpensive model is useful in the education and outreach above all to make the audience more familiar with the parameters of exoplanets (here sizes, distances and partly masses), and it gives new input also for those persons who regularly read papers and news on exoplanets. Keywords: Solar system; Mercury; Jupiter; Exoplanets; Planet; classroom sessions, and two sessions in astronomy camps) with Astrobiology different groups and persons, altogether for 178 participants at these lectures.
    [Show full text]
  • Spin-Orbit Alignment for Three Transiting Hot
    The Astrophysical Journal, 823:29 (16pp), 2016 May 20 doi:10.3847/0004-637X/823/1/29 © 2016. The American Astronomical Society. All rights reserved. SPIN–ORBIT ALIGNMENT FOR THREE TRANSITING HOT JUPITERS: WASP-103b, WASP-87b, and WASP-66b† B. C. Addison1,2, C. G. Tinney1,2, D. J. Wright1,2, and D. Bayliss3 1 Exoplanetary Science Group, School of Physics, University of New South Wales, Sydney, NSW 2052, Australia; [email protected] 2 Australian Centre of Astrobiology, University of New South Wales, Sydney, NSW 2052, Australia 3 Research School of Astronomy and Astrophysics, Australian National University, Canberra, ACT 2611, Australia Received 2015 April 6; accepted 2016 March 16; published 2016 May 18 ABSTRACT We have measured the sky-projected spin–orbit alignments for three transiting hot Jupiters, WASP-103b, WASP- 87b, and WASP-66b, using spectroscopic measurements of the Rossiter–McLaughlin effect, with the CYCLOPS2 optical fiber bundle system feeding the UCLES spectrograph on the Anglo-Australian Telescope. The resulting sky-projected spin–orbit angles of λ=3°±33°, λ=−8°±11°, and λ=−4°±22° for WASP-103b, WASP- 87b, and WASP-66b, respectively, suggest that these three planets are likely on nearly aligned orbits with respect to their host star’s spin axis. WASP-103 is a particularly interesting system as its orbital distance is only 20% larger than its host star’s Roche radius and the planet likely experiences strong tidal effects. WASP-87 and WASP-66 are hot (Teff = 6450 ± 120 K and Teff = 6600 ± 150 K, respectively) mid-F stars, making them similar to the majority of stars hosting planets on high-obliquity orbits.
    [Show full text]