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Where Are the Distant Worlds? Star Maps
W here Are the Distant Worlds? Star Maps Abo ut the Activity Whe re are the distant worlds in the night sky? Use a star map to find constellations and to identify stars with extrasolar planets. (Northern Hemisphere only, naked eye) Topics Covered • How to find Constellations • Where we have found planets around other stars Participants Adults, teens, families with children 8 years and up If a school/youth group, 10 years and older 1 to 4 participants per map Materials Needed Location and Timing • Current month's Star Map for the Use this activity at a star party on a public (included) dark, clear night. Timing depends only • At least one set Planetary on how long you want to observe. Postcards with Key (included) • A small (red) flashlight • (Optional) Print list of Visible Stars with Planets (included) Included in This Packet Page Detailed Activity Description 2 Helpful Hints 4 Background Information 5 Planetary Postcards 7 Key Planetary Postcards 9 Star Maps 20 Visible Stars With Planets 33 © 2008 Astronomical Society of the Pacific www.astrosociety.org Copies for educational purposes are permitted. Additional astronomy activities can be found here: http://nightsky.jpl.nasa.gov Detailed Activity Description Leader’s Role Participants’ Roles (Anticipated) Introduction: To Ask: Who has heard that scientists have found planets around stars other than our own Sun? How many of these stars might you think have been found? Anyone ever see a star that has planets around it? (our own Sun, some may know of other stars) We can’t see the planets around other stars, but we can see the star. -
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. -
Urania Nr 5/2001
Eta Carinae To zdjęcie mgławicy otaczającej gwiazdę // Carinae uzyskano za po mocą telskopu kosmicznego Hubble a (K. Davidson i J. Mors). Porównując je z innymi zdjęciami, a w szczególności z obrazem wyko nanym 17 miesięcy wcześniej, Auto rzy stwierdzili rozprężanie się mgła wicy z szybkością ok. 2,5 min km/h, co prowadzi do wniosku, że rozpo częła ona swe istnienie około 150 lat temu. To bardzo ciekawy i intrygujący wynik. Otóż największy znany roz błysk )j Carinae miał miejsce w roku 1840. Wtedy gwiazda ta stała się naj jaśniejszą gwiazdą południowego nie ba i jasność jej przez krótki czas znacznie przewyższała blask gwiaz dy Canopus. Jednak pyłowy dysk ob serwowany wokół)/ Carinae wydaje się być znacznie młodszy - jego wiek (ekspansji) jest oceniany na 100 lat, co może znaczyć, że powstał w cza sie innego, mniejszego wybuchu ob serwowanego w roku 1890. Więcej na temat tego intrygują cego obiektu przeczytać można we wnątrz numeru, w artykule poświę conym tej gwieździe. NGC 6537 Obserwacje przeprowadzone teleskopem Hubble’a pokazały istnienie wielkich falowych struktur w mgławicy Czerwonego Pająka (NGC 6537) w gwiazdozbiorze Strzelca.Ta gorąca i „wietrzna” mgławica powstała wokół jednej z najgorętszych gwiazd Wszech świata, której wiatr gwiazdowy wiejący z prędkością 2000-4500 kilometrów na sekundę wytwarza fale o wysokości 100 miliardów kilometrów. Sama mgławica rozszerza się z szybkością 300 km/s. Jest też ona wyjątkowo gorąca — ok. 10000 K. Sama gwiazda, która utworzyła mgławicę, jest obecnie białym karłem i musi mieć temperaturę nie niższą niż pół miliona stopni — jest tak gorąca, że nie widać jej w obszarach uzyskanych teleskopem Hubble’a, a świeci głównie w promieniowaniu X. -
AMD-Stability and the Classification of Planetary Systems
A&A 605, A72 (2017) DOI: 10.1051/0004-6361/201630022 Astronomy c ESO 2017 Astrophysics& AMD-stability and the classification of planetary systems? J. Laskar and A. C. Petit ASD/IMCCE, CNRS-UMR 8028, Observatoire de Paris, PSL, UPMC, 77 Avenue Denfert-Rochereau, 75014 Paris, France e-mail: [email protected] Received 7 November 2016 / Accepted 23 January 2017 ABSTRACT We present here in full detail the evolution of the angular momentum deficit (AMD) during collisions as it was described in Laskar (2000, Phys. Rev. Lett., 84, 3240). Since then, the AMD has been revealed to be a key parameter for the understanding of the outcome of planetary formation models. We define here the AMD-stability criterion that can be easily verified on a newly discovered planetary system. We show how AMD-stability can be used to establish a classification of the multiplanet systems in order to exhibit the planetary systems that are long-term stable because they are AMD-stable, and those that are AMD-unstable which then require some additional dynamical studies to conclude on their stability. The AMD-stability classification is applied to the 131 multiplanet systems from The Extrasolar Planet Encyclopaedia database for which the orbital elements are sufficiently well known. Key words. chaos – celestial mechanics – planets and satellites: dynamical evolution and stability – planets and satellites: formation – planets and satellites: general 1. Introduction motion resonances (MMR, Wisdom 1980; Deck et al. 2013; Ramos et al. 2015) could justify the Hill-type criteria, but the The increasing number of planetary systems has made it nec- results on the overlap of the MMR island are valid only for close essary to search for a possible classification of these planetary orbits and for short-term stability. -
Astro-Ph/0611658V3 26 Nov 2006 Ahntn C20015-1305 DC Washington, Ytegnru Nnilspoto H .M Ekfoundation
Four New Exoplanets, and Hints of Additional Substellar Companions to Exoplanet Host Stars1 J. T. Wright2, G. W. Marcy2, D. A Fischer3, R. P. Butler4, S. S. Vogt5, C. G. Tinney6, H. R. A. Jones7, B. D. Carter8, J. A. Johnson2, C. McCarthy3, K. Apps9 ABSTRACT We present four new exoplanets: HIP 14810 b & c, HD 154345 b, and HD 187123 c. The two planets orbiting HIP 14810, from the N2K project, have masses of 3.9 and 0.76 MJup. We have searched the radial velocity time series of 90 known exoplanet systems and found new residual trends due to additional, long period companions. Two stars known to host one exoplanet have sufficient curvature in the residuals to a one planet fit to constrain the minimum mass of the outer companion to be substellar: HD 68988 c with 8 MJup < m sin i< 20 MJup and HD 187123 c with 3MJup < m sin i< 7 MJup, both with P > 8 y. We have also searched the velocity residuals of known exoplanet systems for prospective low-amplitude exoplanets and present some candidates. We discuss techniques for constraining the mass and period of exoplanets in such cases, and for quantifying the significance of weak RV signals. We also present two substellar companions with incomplete orbits and periods longer than 8 y: HD 24040 b and HD 154345 b with m sin i< 20MJup and m sin i< 10 MJup, respectively. Subject headings: planetary systems — techniques: radial velocities 1Based on observations obtained at the W. M. Keck Observatory, which is operated jointly by the Uni- arXiv:astro-ph/0611658v3 26 Nov 2006 versity of California and the California Institute of Technology. -
Superflares and Giant Planets
Superflares and Giant Planets From time to time, a few sunlike stars produce gargantuan outbursts. Large planets in tight orbits might account for these eruptions Eric P. Rubenstein nvision a pale blue planet, not un- bushes to burst into flames. Nor will the lar flares, which typically last a fraction Elike the Earth, orbiting a yellow star surface of the planet feel the blast of ul- of an hour and release their energy in a in some distant corner of the Galaxy. traviolet light and x rays, which will be combination of charged particles, ul- This exercise need not challenge the absorbed high in the atmosphere. But traviolet light and x rays. Thankfully, imagination. After all, astronomers the more energetic component of these this radiation does not reach danger- have now uncovered some 50 “extra- x rays and the charged particles that fol- ous levels at the surface of the Earth: solar” planets (albeit giant ones). Now low them are going to create havoc The terrestrial magnetic field easily de- suppose for a moment something less when they strike air molecules and trig- flects the charged particles, the upper likely: that this planet teems with life ger the production of nitrogen oxides, atmosphere screens out the x rays, and and is, perhaps, populated by intelli- which rapidly destroy ozone. the stratospheric ozone layer absorbs gent beings, ones who enjoy looking So in the space of a few days the pro- most of the ultraviolet light. So solar up at the sky from time to time. tective blanket of ozone around this flares, even the largest ones, normally During the day, these creatures planet will largely disintegrate, allow- pass uneventfully. -
June 2006.Indd
San Diego Astronomy Association Celebrating Over 40 Years of Astronomical Outreach Offi ce (619) 645-8940 June 2006 Observatory (619) 766-9118 NASA’s Night Sky Network http://www.sdaa.org A Non-Profi t Educational Association Show Me the Planets P.O. Box 23215, San Diego, CA 92193-3215 by Mark Smith In this season of great planet watching, I thought it might be fun to explore some SDAA Business Meeting planets a little farther afi eld. It is not unusual to be asked about planets around other Next meeting will be held at: stars at a star party and it is nice to be able to talk about this subject in a way that Teledyne RD Instruments USA makes sense to the average person. After all, the most basic question that drives all 9855 Businesspark Avenue of astronomy is, “What’s out there?” and extrasolar planets are the “what” that most San Diego, CA, USA 92131-1101 captures the imagination of the average person. June 13th at 7:00 pm Unfortunately, talk about measuring the wobble of stars with Doppler shifts or looking for the drop in brightness due to a transiting planet does not mean much to Next Program Meeting the average person. Fortunately, you can explain, and even demonstrate, the most The Problem with Pluto important concepts of the search for extrasolar planets using nothing more than a by Dr. Gary Peterson three inch diameter foam squishy ball and a golf tee. If you add a small rubber ball June 21st at 7:00 pm glued to the fl at end of the golf tee, you are really set! Simply stick the golf tee about Mission Trails Regional Park a third of the way into the squishy ball and you are ready to begin. -
Planetquest Outreach Toolkit Manual and Resources Cd
Outreach ToolKit Manual DISTRIBUTED FOR MEMBERS OF THE NASA NIGHT SKY NETWORK THE NIGHT SKY NETWORK IS SPONSORED AND SUPPORTED BY JPL'S PLANETQUEST PUBLIC ENGAGEMENT PROGRAM. PLANETQUEST IS A PART OF JPL’S NAVIGATOR PROGRAM, WHICH ENCOMPASSES SEVERAL OF NASA'S EXTRA-SOLAR PLANET- FINDING MISSIONS, INCLUDING THE KECK INTERFEROMETER, THE SPACE INTERFEROMETRY MISSION (SIM), THE TERRESTRIAL PLANET FINDER (TPF), THE LARGE BINOCULAR TELESCOPE INTERFEROMETER (LBTI), AND THE MICHELSON SCIENCE CENTER. NASA NIGHT SKY NETWORK: http://nightsky.jpl.nasa.gov/ PLANETQUEST: http://planetquest.jpl.nasa.gov/ Contacts The non-profit Astronomical Society of the Pacific (ASP), one of the nation’s leading organizations devoted to astronomy and space science education, is managing the Night Sky Network in cooperation with JPL. Learn more about the ASP at http://www.astrosociety.org. For support contact: Astronomical Society of the Pacific (ASP) 390 Ashton Avenue San Francisco, CA 94112 415-337-1100 ext. 116 [email protected] Copyright © 2004 NASA/JPL and Astronomical Society of the Pacific. Copies of this manual and documents may be made for educational and public outreach purposes only and are to be supplied at no charge to participants. Any other use is not permitted. CREDITS: All photos and images in the ToolKit Manual unless otherwise noted are provided courtesy of Marni Berendsen and Rich Berendsen. Your Club’s Membership in the NASA Night Sky Network Welcome to the NASA Night Sky Network! Your membership in the Night Sky Network will provide many opportunities for your club to expand its public education and outreach. Your club has at least two members who are the Night Sky Network Club Coordinators. -
Statistical Properties of Exoplanets
A&A 398, 363–376 (2003) Astronomy DOI: 10.1051/0004-6361:20021637 & c ESO 2003 Astrophysics Statistical properties of exoplanets II. Metallicity, orbital parameters, and space velocities N. C. Santos1, G. Israelian2, M. Mayor1,R.Rebolo2,3,andS.Udry1 1 Observatoire de Gen`eve, 51 ch. des Maillettes, 1290 Sauverny, Switzerland 2 Instituto de Astrof´ısica de Canarias, 38200 La Laguna, Tenerife, Spain 3 Consejo Superior de Investigaciones Cient´ıficas, Spain Received 19 September 2002 / Accepted 7 November 2002 Abstract. In this article we present a detailed spectroscopic analysis of more than 50 extra-solar planet host stars. Stellar atmospheric parameters and metallicities are derived using high resolution and high S/N spectra. The spectroscopy results, added to the previous studies, imply that we have access to a large and uniform sample of metallicities for about 80 planet hosts stars. We make use of this sample to confirm the metal-rich nature of stars with planets, and to show that the planetary frequency is rising as a function of the [Fe/H]. Furthermore, the source of this high metallicity is shown to have most probably a “primordial” source, confirming previous results. The comparison of the orbital properties (period and eccentricity) and minimum masses of the planets with the stellar properties also reveal some emerging but still not significant trends. These are discussed and some explanations are proposed. Finally, we show that the planet host stars included in the CORALIE survey have similar kinematical properties as the whole CORALIE volume-limited planet search sample. Planet hosts simply seem to occupy the metal-rich envelope of this latter population. -