400 Years of Women in Science Review by Andrew W
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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. -
Download the Search for New Planets
“VITAL ARTICLES ON SCIENCE/CREATION” September 1999 Impact #315 THE SEARCH FOR NEW PLANETS by Don DeYoung, Ph.D.* The nine solar system planets, from Mercury to Pluto, have been much-studied targets of the space age. In general, a planet is any massive object which orbits a star, in our case, the Sun. Some have questioned the status of Pluto, mainly because of its small size, but it remains a full-fledged planet. There is little evidence for additional solar planets beyond Pluto. Instead, attention has turned to extrasolar planets which may circle other stars. Intense competition has arisen among astronomers to detect such objects. Success insures media attention, journal publication, and continued research funding. The Interest in Planets Just one word explains the intense interest in new planets—life. Many scientists are convinced that we are not alone in space. Since life evolved on Earth, it must likewise have happened elsewhere, either on planets or their moons. The naïve assumption is that life will arise if we “just add water”: Earth-like planet + water → spontaneous life This equation is falsified by over a century of biological research showing the deep complexity of life. Scarcely is there a fact more certain than that matter does not spring into life on its own. Drake Equation Astronomer Frank Drake pioneered the Search for ExtraTerrestrial Intelligence project, or SETI, in the 1960s. He also attempted to calculate the total number of planets with life. The Drake Equation in simplified form is: Total livable Probability of Planets with planets x evolution = evolved life *Don DeYoung, Ph.D., is an Adjunct Professor of Physics at ICR. -
Today in Astronomy 106: Exoplanets
Today in Astronomy 106: exoplanets The successful search for extrasolar planets Prospects for determining the fraction of stars with planets, and the number of habitable planets per planetary system (fp and ne). T. Pyle, SSC/JPL/Caltech/NASA. 26 May 2011 Astronomy 106, Summer 2011 1 Observing exoplanets Stars are vastly brighter and more massive than planets, and most stars are far enough away that the planets are lost in the glare. So astronomers have had to be more clever and employ the motion of the orbiting planet. The methods they use (exoplanets detected thereby): Astrometry (0): tiny wobble in star’s motion across the sky. Radial velocity (399): tiny wobble in star’s motion along the line of sight by Doppler shift. Timing (9): tiny delay or advance in arrival of pulses from regularly-pulsating stars. Gravitational microlensing (10): brightening of very distant star as it passes behind a planet. 26 May 2011 Astronomy 106, Summer 2011 2 Observing exoplanets (continued) Transits (69): periodic eclipsing of star by planet, or vice versa. Very small effect, about like that of a bug flying in front of the headlight of a car 10 miles away. Imaging (11 but 6 are most likely to be faint stars): taking a picture of the planet, usually by blotting out the star. Of these by far the most useful so far has been the combination of radial-velocity and transit detection. Astrometry and gravitational microlensing of sufficient precision to detect lots of planets would need dedicated, specialized observatories in space. Imaging lots of planets will require 30-meter-diameter telescopes for visible and infrared wavelengths. -
IAU Division C Working Group on Star Names 2019 Annual Report
IAU Division C Working Group on Star Names 2019 Annual Report Eric Mamajek (chair, USA) WG Members: Juan Antonio Belmote Avilés (Spain), Sze-leung Cheung (Thailand), Beatriz García (Argentina), Steven Gullberg (USA), Duane Hamacher (Australia), Susanne M. Hoffmann (Germany), Alejandro López (Argentina), Javier Mejuto (Honduras), Thierry Montmerle (France), Jay Pasachoff (USA), Ian Ridpath (UK), Clive Ruggles (UK), B.S. Shylaja (India), Robert van Gent (Netherlands), Hitoshi Yamaoka (Japan) WG Associates: Danielle Adams (USA), Yunli Shi (China), Doris Vickers (Austria) WGSN Website: https://www.iau.org/science/scientific_bodies/working_groups/280/ WGSN Email: [email protected] The Working Group on Star Names (WGSN) consists of an international group of astronomers with expertise in stellar astronomy, astronomical history, and cultural astronomy who research and catalog proper names for stars for use by the international astronomical community, and also to aid the recognition and preservation of intangible astronomical heritage. The Terms of Reference and membership for WG Star Names (WGSN) are provided at the IAU website: https://www.iau.org/science/scientific_bodies/working_groups/280/. WGSN was re-proposed to Division C and was approved in April 2019 as a functional WG whose scope extends beyond the normal 3-year cycle of IAU working groups. The WGSN was specifically called out on p. 22 of IAU Strategic Plan 2020-2030: “The IAU serves as the internationally recognised authority for assigning designations to celestial bodies and their surface features. To do so, the IAU has a number of Working Groups on various topics, most notably on the nomenclature of small bodies in the Solar System and planetary systems under Division F and on Star Names under Division C.” WGSN continues its long term activity of researching cultural astronomy literature for star names, and researching etymologies with the goal of adding this information to the WGSN’s online materials. -
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. -
Downloads/ Astero2007.Pdf) and by Aerts Et Al (2010)
This work is protected by copyright and other intellectual property rights and duplication or sale of all or part is not permitted, except that material may be duplicated by you for research, private study, criticism/review or educational purposes. Electronic or print copies are for your own personal, non- commercial use and shall not be passed to any other individual. No quotation may be published without proper acknowledgement. For any other use, or to quote extensively from the work, permission must be obtained from the copyright holder/s. i Fundamental Properties of Solar-Type Eclipsing Binary Stars, and Kinematic Biases of Exoplanet Host Stars Richard J. Hutcheon Submitted in accordance with the requirements for the degree of Doctor of Philosophy. Research Institute: School of Environmental and Physical Sciences and Applied Mathematics. University of Keele June 2015 ii iii Abstract This thesis is in three parts: 1) a kinematical study of exoplanet host stars, 2) a study of the detached eclipsing binary V1094 Tau and 3) and observations of other eclipsing binaries. Part I investigates kinematical biases between two methods of detecting exoplanets; the ground based transit and radial velocity methods. Distances of the host stars from each method lie in almost non-overlapping groups. Samples of host stars from each group are selected. They are compared by means of matching comparison samples of stars not known to have exoplanets. The detection methods are found to introduce a negligible bias into the metallicities of the host stars but the ground based transit method introduces a median age bias of about -2 Gyr. -
3-D Starmap 15.0 All Stars Within 15 Parsecs (50 Light-Years) of Sol
3-D Starmap 15.0 All stars within 15 parsecs (50 light-years) of Sol. Gl 815 2.0:14.9:-1.0 All units are in parsecs. (1 parsec = 3.26 light-years) 1.5 Gl 792 Stars are plotted in cartesian x,y,z coordinates. 3.2:14.7:-0.2 X-Y plane is the plane of the galaxy. Alderamin 2.3 -2.8:14.5:2.4 +x is Coreward, -x is Rimward, NN 4276 -3.9:14.4:0.4 +y is Spinward, -y is Trailing 1.2 Star data is from HYG database. 3.2 Stars circled in green are likely to host 14.0 human-habitable planets, according to 3 Eta Cephei 1.3 -1.9:13.9:2.9 the HabCat database. Gray lines link each star with its two closest neighbors. 2.9 3.0 Green lines link habitable stars with their two Hip 101516 5.7:13.5:-2.3 closest habitable neighbors. NN 4338 B GJ 1228 -4.1:13.4:-4.8 3.0 1.5:13.4:6.2 Gl 878 2.6 GJ 1270 0.4 Links are labeled with their distance in parsecs. -4.6:13.3:0.3 -1.5:13.3:-3.3 3.1 2.6 Gl 794 NN 4109 Winchell Chung: Nyrath the nearly wise 5.5:13.1:-2.3 2.0 7.0:13.1:1.5 http://www.projectrho.com/starmap.html 13.0 Gl 738 2.3 6.5:13.0:3.4 Gl 875.1 1.9 -1.2:12.9:-5.9 2.2 1.5 1.6 2.2 2.7 NN 4073 4.6:12.6:4.5 Gl 14 -6.1:12.5:-5.5 Gl 52 2.6 Gl 806 -28..6:12.4:0.3 1.3:12.4:0.2 4.4 3.8 NN 3069 BD+27°4120 2.6 Gl 813 BD+31°3767 -8.5:12.3:-2.3 2.4:12.3:-4.1 4.9:12.3:-3.55.1:12.3:0.8 BD+57°2735 -4.8:12.2:-0.7 19 Draconis -1.2:12.1:9.0 1.7 12.0 2.1 1.3 Gl 742 26 Draconis NN 4228 3.0 -2.4:11.9:5.6 -0.2:11.9:7.6 4.3:11.6.9:-7.4 1.1 2.5 3.8 1.7 2.4 1.9 35 Gamma Cephei GJ 1243 2.1 2.9 -6.4:11.6:3.6 1.9:11.6:2.1 NN 3117 2.3 NN 4040 2.8 -9.5:11.5:0.6 1.9 2.1 4.1 3.4:11.5:6.4 -
Arxiv:2010.00015V3 [Hep-Ph] 26 Apr 2021 Galactic Halo Can Scatter with Exoplanets, Lose Energy, and Gles Are the Same Set of Planets, Without DM Heating
MIT-CTP/5230 SLAC-PUB-17556 Exoplanets as Sub-GeV Dark Matter Detectors Rebecca K. Leane1, 2, ∗ and Juri Smirnov3, 4, y 1Center for Theoretical Physics, Massachusetts Institute of Technology, Cambridge, MA 02139, USA 2SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94039, USA 3Center for Cosmology and AstroParticle Physics (CCAPP), The Ohio State University, Columbus, OH 43210, USA 4Department of Physics, The Ohio State University, Columbus, OH 43210, USA (Dated: April 27, 2021) We present exoplanets as new targets to discover Dark Matter (DM). Throughout the Milky Way, DM can scatter, become captured, deposit annihilation energy, and increase the heat flow within exoplanets. We estimate upcoming infrared telescope sensitivity to this scenario, finding actionable discovery or exclusion searches. We find that DM with masses above about an MeV can be probed with exoplanets, with DM-proton and DM-electron scattering cross sections down to about 10−37cm2, stronger than existing limits by up to six orders of magnitude. Supporting evidence of a DM origin can be identified through DM-induced exoplanet heating correlated with Galactic position, and hence DM density. This provides new motivation to measure the temperature of the billions of brown dwarfs, rogue planets, and gas giants peppered throughout our Galaxy. Introduction{Are we alone in the Universe? This ques- Exoplanet Temperatures tion has driven wide-reaching interest in discovering a 104 planet like our own. Regardless of whether or not we ever find alien life, the scientific advances from finding DM Heating and understanding other planets will be enormous. From a particle physics perspective, new celestial bodies pro- vide a vast playground to discover new physics. -
Williams & Kasting, 1997
ICARUS 129, 254±267 (1997) ARTICLE NO. IS975759 Habitable Planets with High Obliquities1 Darren M. Williams Department of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Laboratory, University Park, Pennsylvania 16802 E-mail: [email protected] and James F. Kasting Department of Geosciences, Pennsylvania State University, 211 Deike Building, University Park, Pennsylvania 16802 Received September 19, 1996; revised April 21, 1997 Butler and Marcy 1996, Gatewood 1996, Butler et al. 1996, Earth's obliquity would vary chaotically from 08 to 858 were Cochran et al. 1996) have generated widespread anticipa- it not for the presence of the Moon (J. Laskar, F. Joutel, and tion of detecting an Earth-like planet around a nearby P. Robutel, 1993, Nature 361, 615±617). The Moon itself is solar-type star. As of this writing, all of the companions thought to be an accident of accretion, formed by a glancing found around Sun-like main-sequence stars are at least 1.5 blow from a Mars-sized planetesimal. Hence, planets with simi- times the mass of Saturn, and none of these objects orbit lar moons and stable obliquities may be extremely rare. This entirely within a circumstellar habitable zone, or HZ (Wil- has lead Laskar and colleagues to suggest that the number of Earth-like planets with high obliquities and temperate, life- liams et al. 1997). We follow Kasting et al. (1993, henceforth supporting climates may be small. KWR) in de®ning the HZ as the region around a star in To test this proposition, we have used an energy-balance which an Earth-like planet (of comparable mass and having climate model to simulate Earth's climate at obliquities up to an atmosphere containing N2 ,H2O, and CO2) is climati- 908. -
P Lanetary Postc Ards
Suggested Discussion Questions for Planetary PostCards That star is hotter/colder than our Sun. How do you Planetary PostCards think that might affect its planets? Here is where one of the planets orbits that star. What would it be like to live on this planet (or one of its moons)? If Earth was orbiting that star, what might be different? Artist: Lynette Cook 55 Cancri System How big do you suppose this planet is compared to Abbreviations and terms used on PostCards the planets in our Solar System? RA = Right Ascension Do you think we have found all the planets in this Dec = Declination system? mag = apparent visual magnitude AU = Astronomical Unit, the distance between the Earth and Our fastest spacecraft travels 42 miles per second. It the Sun: 93 million miles or 150 million km would take 5,000 years for that spacecraft to go one Light year = The distance light travels in a year. Light travels at light year. How long would it take to reach this star 186,000 miles per second or 300,000 km per second. Light which is ____ light years away? from the Sun takes 8 minutes to reach Earth. Jupiter mass = 1.9 x1027 kg. Jupiter is about 300 times more How different do you think Earth will be in that massive than Earth (approximate difference between a large period of time? bowling ball and a small marble) Temperature of the stars is in degrees Celsius Cepheus Draco Ursa Ursa Minor gamma Cephei 39' º mag: 3.2 mag: Dec: 77 Dec: RA: 23h 39m RA: Ursa MajorUrsa Star: Gamma Cephei Planet: Gamma Cephei b Star’s System Compared to Our Solar System How far in How Hot? light years? °C Neptune 150 7000 Uranus < Sun 100 Saturn Star > 5000 Gamma Cephei b > 50 3000 Jupiter < 39 < Companion Star Sun 1000 Planet (year discovered): b (2002) The brightest star with a planet is Avg Distance From Star: 2 AU (Earth from Sun = 1 AU) a Binary star AND it’s a Red Giant! Orbit: Its small “companion star” gets as 2.5 years close as 12 AU in a 40-year orbit. -
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.