MPE 1963 – 2013 Reflections on 50 Years of Extraterrestrial Research
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WARP Ten, 1992 Columbia College Chicago
Columbia College Chicago Digital Commons @ Columbia College Chicago WARP ten Publications 2-1-1992 WARP ten, 1992 Columbia College Chicago Follow this and additional works at: https://digitalcommons.colum.edu/warpten Part of the Journalism Studies Commons This work is licensed under a Creative Commons Attribution-Noncommercial-No Derivative Works 4.0 License. Recommended Citation Columbia College Chicago, "WARP ten, 1992" (1992). WARP ten. 1. https://digitalcommons.colum.edu/warpten/1 This Book is brought to you for free and open access by the Publications at Digital Commons @ Columbia College Chicago. It has been accepted for inclusion in WARP ten by an authorized administrator of Digital Commons @ Columbia College Chicago. For more information, please contact [email protected]. A Science Newsletter of Columbia College Journalism Department Vol.I , No.I -~ Of Mars and Men By Robbie Robb the moon, a distance of 384,000km (239,000 miles) is but a three day voyage. A one-way trip to Mars, a distance of 56.4 million km. (35 million miles) rcquimi 280 days. The sheec The lure of the red planet has tantalized hlJIJUlllity for cen scope of the project thus demands a more expensive turies. Authors from H. G. Wells to Ray Bradbury havewriucn spacecraft. But traveling to Mars would also require more about life on Mars and coloni2ation of the planet. The Arnold resources at additional cosl Vast arnounlS of supplies, food. Schwanznegger movie, "Total Recall," portrayed a Martilln equipment, and fuel would be needed for a trip of this m11& world inhabited by tran.splanted earthlings. Now the idea of nitude. -
Photochemically Driven Collapse of Titan's Atmosphere
REPORTS has escaped, the surface temperature again Photochemically Driven Collapse decreases, down to about 86 K, slightly of Titan’s Atmosphere above the equilibrium temperature, because of the slight greenhouse effect resulting Ralph D. Lorenz,* Christopher P. McKay, Jonathan I. Lunine from the N2 opacity below (longward of) 200 cm21. Saturn’s giant moon Titan has a thick (1.5 bar) nitrogen atmosphere, which has a These calculations assume the present temperature structure that is controlled by the absorption of solar and thermal radiation solar constant of 15.6 W m22 and a surface by methane, hydrogen, and organic aerosols into which methane is irreversibly converted albedo of 0.2 and ignore the effects of N2 by photolysis. Previous studies of Titan’s climate evolution have been done with the condensation. As noted in earlier studies assumption that the methane abundance was maintained against photolytic depletion (5), when the atmosphere cools during the throughout Titan’s history, either by continuous supply from the interior or by buffering CH4 depletion, the model temperature at by a surface or near surface reservoir. Radiative-convective and radiative-saturated some altitudes in the atmosphere (here, at equilibrium models of Titan’s atmosphere show that methane depletion may have al- ;10 km for 20% CH4 surface humidity) lowed Titan’s atmosphere to cool so that nitrogen, its main constituent, condenses onto becomes lower than the saturation temper- the surface, collapsing Titan into a Triton-like frozen state with a thin atmosphere. -
Detection of Large-Scale X-Ray Bubbles in the Milky Way Halo
Detection of large-scale X-ray bubbles in the Milky Way halo P. Predehl1†, R. A. Sunyaev2,3†, W. Becker1,4, H. Brunner1, R. Burenin2, A. Bykov5, A. Cherepashchuk6, N. Chugai7, E. Churazov2,3†, V. Doroshenko8, N. Eismont2, M. Freyberg1, M. Gilfanov2,3†, F. Haberl1, I. Khabibullin2,3, R. Krivonos2, C. Maitra1, P. Medvedev2, A. Merloni1†, K. Nandra1†, V. Nazarov2, M. Pavlinsky2, G. Ponti1,9, J. S. Sanders1, M. Sasaki10, S. Sazonov2, A. W. Strong1 & J. Wilms10 1Max-Planck-Institut für Extraterrestrische Physik, Garching, Germany. 2Space Research Institute of the Russian Academy of Sciences, Moscow, Russia. 3Max-Planck-Institut für Astrophysik, Garching, Germany. 4Max-Planck-Institut für Radioastronomie, Bonn, Germany. 5Ioffe Institute, St Petersburg, Russia. 6M. V. Lomonosov Moscow State University, P. K. Sternberg Astronomical Institute, Moscow, Russia. 7Institute of Astronomy, Russian Academy of Sciences, Moscow, Russia. 8Institut für Astronomie und Astrophysik, Tübingen, Germany. 9INAF-Osservatorio Astronomico di Brera, Merate, Italy. 10Dr. Karl-Remeis-Sternwarte Bamberg and ECAP, Universität Erlangen-Nürnberg, Bamberg, Germany. †e-mail: [email protected]; [email protected]; [email protected]; [email protected]; [email protected]; [email protected] The halo of the Milky Way provides a laboratory to study the properties of the shocked hot gas that is predicted by models of galaxy formation. There is observational evidence of energy injection into the halo from past activity in the nucleus of the Milky Way1–4; however, the origin of this energy (star formation or supermassive-black-hole activity) is uncertain, and the causal connection between nuclear structures and large-scale features has not been established unequivocally. -
On the Possibility of Registering X-Ray Flares Related to Fast Radio
On the possibility of registering X-ray flares related to fast radio bursts with the SRG/eROSITA telescope A.D. Khokhryakova1, D.A. Lyapina1, S.B. Popov1;2;3 1 Department of Physics, Lomonosov Moscow State University 2 Sternberg Astronomical Institute, Lomonosov Moscow State University 3 Higher School of Economics, Moscow March 27, 2019 Abstract In this note we discuss the possibility of detecting the accompanying X-ray emission from sources of fast radio bursts with the eROSITA telescope on- board the Spektr-RG observatory. It is shown that during four years of the survey program about 300 bursts are expected to appear in the field of view of eROSITA. About 1% of them will be detected by ground-based radio tele- scopes. For a total energy release ∼ 1046 ergs depending on the spectral parameters and absorption in the interstellar and intergalactic media, an X- ray flare can be detected from distances from ∼ 1 Mpc (thermal spectrum with kT = 200 keV and strong absorption) up to ∼ 1 Gpc (power-law spec- trum with photon index Γ = 2 and realistic absorption). Thus, eROSITA observations might help to provide important constraints on parameters of arXiv:1903.10991v1 [astro-ph.HE] 26 Mar 2019 sources of fast radio bursts, or may even allow to identify the X-ray tran- sient counterparts, which will help to constrain models of fast radio bursts generation. 1 1 Introduction Fast radio bursts (FRBs) are short (∼ms) bright (peak fluxes up to ∼100 Jy) radio flashes (for a review, see [1]).1 The first event from this class of tran- sients was introduced in 2007 in [2]. -
Light, Color, and Atmospheric Optics
Light, Color, and Atmospheric Optics GEOL 1350: Introduction To Meteorology 1 2 • During the scattering process, no energy is gained or lost, and therefore, no temperature changes occur. • Scattering depends on the size of objects, in particular on the ratio of object’s diameter vs wavelength: 1. Rayleigh scattering (D/ < 0.03) 2. Mie scattering (0.03 ≤ D/ < 32) 3. Geometric scattering (D/ ≥ 32) 3 4 • Gas scattering: redirection of radiation by a gas molecule without a net transfer of energy of the molecules • Rayleigh scattering: absorption extinction 4 coefficient s depends on 1/ . • Molecules scatter short (blue) wavelengths preferentially over long (red) wavelengths. • The longer pathway of light through the atmosphere the more shorter wavelengths are scattered. 5 • As sunlight enters the atmosphere, the shorter visible wavelengths of violet, blue and green are scattered more by atmospheric gases than are the longer wavelengths of yellow, orange, and especially red. • The scattered waves of violet, blue, and green strike the eye from all directions. • Because our eyes are more sensitive to blue light, these waves, viewed together, produce the sensation of blue coming from all around us. 6 • Rayleigh Scattering • The selective scattering of blue light by air molecules and very small particles can make distant mountains appear blue. The blue ridge mountains in Virginia. 7 • When small particles, such as fine dust and salt, become suspended in the atmosphere, the color of the sky begins to change from blue to milky white. • These particles are large enough to scatter all wavelengths of visible light fairly evenly in all directions. -
Report of Contributions
Mapping the X-ray Sky with SRG: First Results from eROSITA and ART-XC Report of Contributions https://events.mpe.mpg.de/e/SRG2020 Mapping the X- … / Report of Contributions eROSITA discovery of a new AGN … Contribution ID : 4 Type : Oral Presentation eROSITA discovery of a new AGN state in 1H0707-495 Tuesday, 17 March 2020 17:45 (15) One of the most prominent AGNs, the ultrasoft Narrow-Line Seyfert 1 Galaxy 1H0707-495, has been observed with eROSITA as one of the first CAL/PV observations on October 13, 2019 for about 60.000 seconds. 1H 0707-495 is a highly variable AGN, with a complex, steep X-ray spectrum, which has been the subject of intense study with XMM-Newton in the past. 1H0707-495 entered an historical low hard flux state, first detected with eROSITA, never seen before in the 20 years of XMM-Newton observations. In addition ultra-soft emission with a variability factor of about 100 has been detected for the first time in the eROSITA light curves. We discuss fast spectral transitions between the cool and a hot phase of the accretion flow in the very strong GR regime as a physical model for 1H0707-495, and provide tests on previously discussed models. Presenter status Senior eROSITA consortium member Primary author(s) : Prof. BOLLER, Thomas (MPE); Prof. NANDRA, Kirpal (MPE Garching); Dr LIU, Teng (MPE Garching); MERLONI, Andrea; Dr DAUSER, Thomas (FAU Nürnberg); Dr RAU, Arne (MPE Garching); Dr BUCHNER, Johannes (MPE); Dr FREYBERG, Michael (MPE) Presenter(s) : Prof. BOLLER, Thomas (MPE) Session Classification : AGN physics, variability, clustering October 3, 2021 Page 1 Mapping the X- … / Report of Contributions X-ray emission from warm-hot int … Contribution ID : 9 Type : Poster X-ray emission from warm-hot intergalactic medium: the role of resonantly scattered cosmic X-ray background We revisit calculations of the X-ray emission from warm-hot intergalactic medium (WHIM) with particular focus on contribution from the resonantly scattered cosmic X-ray background (CXB). -
Project Horizon Report
Volume I · SUMMARY AND SUPPORTING CONSIDERATIONS UNITED STATES · ARMY CRD/I ( S) Proposal t c• Establish a Lunar Outpost (C) Chief of Ordnance ·cRD 20 Mar 1 95 9 1. (U) Reference letter to Chief of Ordnance from Chief of Research and Devel opment, subject as above. 2. (C) Subsequent t o approval by t he Chief of Staff of reference, repre sentatives of the Army Ballistic ~tissiles Agency indicat e d that supplementar y guidance would· be r equired concerning the scope of the preliminary investigation s pecified in the reference. In particular these r epresentatives requested guidance concerning the source of funds required to conduct the investigation. 3. (S) I envision expeditious development o! the proposal to establish a lunar outpost to be of critical innportance t o the p. S . Army of the future. This eva luation i s appar ently shar ed by the Chief of Staff in view of his expeditious a pproval and enthusiastic endorsement of initiation of the study. Therefore, the detail to be covered by the investigation and the subs equent plan should be as com plete a s is feas ible in the tin1e limits a llowed and within the funds currently a vailable within t he office of t he Chief of Ordnance. I n this time of limited budget , additional monies are unavailable. Current. programs have been scrutinized r igidly and identifiable "fat'' trimmed awa y. Thus high study costs are prohibitive at this time , 4. (C) I leave it to your discretion t o determine the source and the amount of money to be devoted to this purpose. -
Erosita – Mapping the X-Ray Universe by P. Predehl
Astron. Nachr. /AN 335, No. 5, 517 – 522 (2014) / DOI 10.1002/asna.201412059 eROSITA – Mapping the X-ray universe P. Predehl Max-Planck-Institut f¨ur extraterrestrische Physik, Giessenbachstraße, D-85748 Garching, Germany Received 2014 Apr 7, accepted 2014 Apr 10 Published online 2014 Jun 2 Key words space vehicles – surveys – telescopes – X-rays: general eROSITA (extended ROentgen Survey with an Imaging Telescope Array) is the core instrument on the Russian/German Spektrum-Roentgen-Gamma (SRG) mission which is currently scheduled for launch late 2015/early 2016. eROSITA will perform a deep survey of the entire X-ray sky. In the soft band (0.5–2 keV), it will be about 30 times more sensitive than ROSAT, while in the hard band (2–8 keV) it will provide the first ever true imaging survey of the sky. The design driving science is the detection of large samples of galaxy clusters to redshifts z>1 in order to study the large scale structure in the universe and test cosmological models including dark energy. In addition, eROSITA is expected to yield a sample of a few million active galactic nuclei, including obscured objects, revolutionizing our view of the evolution of supermassive black holes. The survey will also provide new insights into a wide range of astrophysical phenomena, including X-ray binaries, active stars, and diffuse emission within the Galaxy. eROSITA is currently (Jan 2014) in its flight model and calibration phase. All seven flight mirror modules (plus one spare) have been delivered and measured in X-rays. The first camera including the complete electronics has been extensively tested. -
SRGA J124404. 1-632232/SRGU J124403. 8-632231: a New X-Ray
Astronomy & Astrophysics manuscript no. main ©ESO 2021 June 29, 2021 SRGA J124404.1−632232/SRGU J124403.8−632231: a new X-ray pulsar discovered in the all-sky survey by SRG V.Doroshenko1, R. Staubert1, C. Maitra2, A. Rau2, F. Haberl2, A. Santangelo1, A. Schwope3, J. Wilms4, D.A.H. Buckley5; 6, A. Semena7, I. Mereminskiy7, A. Lutovinov7, M. Gromadzki8, L.J. Townsend5; 9, I.M. Monageng5; 6 1 Institut für Astronomie und Astrophysik, Sand 1, 72076 Tübingen, Germany 2 Max-Planck-Institut für extraterrestrische Physik, Gießenbachstraße 1, 85748 Garching, Germany 3 Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, 14482 Potsdam, Germany 4 Dr. Karl Remeis-Sternwarte and Erlangen Centre for Astroparticle Physics, Friedrich-Alexander-Universität Erlangen-Nürnberg, Sternwartstr. 7, 96049 Bamberg, Germany 5 South African Astronomical Observatory, PO Box 9, Observatory Rd, Observatory 7935, South Africa 6 Department of Astronomy, University of Cape Town, Private Bag X3, Rondebosch 7701, South Africa 7 Space Research Institute (IKI) of Russian Academy of Sciences, Prosoyuznaya ul 84/32, 117997 Moscow, Russian Federation 8 Astronomical Observatory, University of Warsaw, Al. Ujazdowskie 4, 00-478 Warsaw, Poland 9 Southern African Large Telescope, PO Box 9, Observatory Rd, Observatory 7935, South Africa June 29, 2021 ABSTRACT Ongoing all-sky surveys by the the eROSITA and the Mikhail Pavlinsky ART-XC telescopes on-board the Spec- trum Roentgen Gamma (SRG) mission have already revealed over a million of X-ray sources. One of them, SRGA J124404.1−632232/SRGU J124403.8−632231, was detected as a new source in the third (of the planned eight) consecu- tive X-ray surveys by ART-XC. -
Links to Education Standards • Introduction to Exoplanets • Glossary of Terms • Classroom Activities Table of Contents Photo © Michael Malyszko Photo © Michael
an Educator’s Guid E INSIDE • Links to Education Standards • Introduction to Exoplanets • Glossary of Terms • Classroom Activities Table of Contents Photo © Michael Malyszko Photo © Michael For The TeaCher About This Guide .............................................................................................................................................. 4 Connections to Education Standards ................................................................................................... 5 Show Synopsis .................................................................................................................................................. 6 Meet the “Stars” of the Show .................................................................................................................... 8 Introduction to Exoplanets: The Basics .................................................................................................. 9 Delving Deeper: Teaching with the Show ................................................................................................13 Glossary of Terms ..........................................................................................................................................24 Online Learning Tools ..................................................................................................................................26 Exoplanets in the News ..............................................................................................................................27 During -
The X-Ray Imaging Polarimetry Explorer
Call for a Medium-size mission opportunity in ESA‟s Science Programme for a launch in 2025 (M4) XXIIPPEE The X-ray Imaging Polarimetry Explorer Lead Proposer: Paolo Soffitta (INAF-IAPS, Italy) Contents 1. Executive summary ................................................................................................................................................ 3 2. Science case ........................................................................................................................................................... 5 3. Scientific requirements ........................................................................................................................................ 15 4. Proposed scientific instruments............................................................................................................................ 20 5. Proposed mission configuration and profile ........................................................................................................ 35 6. Management scheme ............................................................................................................................................ 45 7. Costing ................................................................................................................................................................. 50 8. Annex ................................................................................................................................................................... 52 Page 1 XIPE is proposed -
Atmospheric Optics
53 Atmospheric Optics Craig F. Bohren Pennsylvania State University, Department of Meteorology, University Park, Pennsylvania, USA Phone: (814) 466-6264; Fax: (814) 865-3663; e-mail: [email protected] Abstract Colors of the sky and colored displays in the sky are mostly a consequence of selective scattering by molecules or particles, absorption usually being irrelevant. Molecular scattering selective by wavelength – incident sunlight of some wavelengths being scattered more than others – but the same in any direction at all wavelengths gives rise to the blue of the sky and the red of sunsets and sunrises. Scattering by particles selective by direction – different in different directions at a given wavelength – gives rise to rainbows, coronas, iridescent clouds, the glory, sun dogs, halos, and other ice-crystal displays. The size distribution of these particles and their shapes determine what is observed, water droplets and ice crystals, for example, resulting in distinct displays. To understand the variation and color and brightness of the sky as well as the brightness of clouds requires coming to grips with multiple scattering: scatterers in an ensemble are illuminated by incident sunlight and by the scattered light from each other. The optical properties of an ensemble are not necessarily those of its individual members. Mirages are a consequence of the spatial variation of coherent scattering (refraction) by air molecules, whereas the green flash owes its existence to both coherent scattering by molecules and incoherent scattering