Classification of Interstellar Radio Messages
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A Direct Communication Proposal to Test the Zoo Hypothesis
Space Policy 38 (2016) 22e26 Contents lists available at ScienceDirect Space Policy journal homepage: www.elsevier.com/locate/spacepol Viewpoint A direct communication proposal to test the Zoo Hypothesis Joao~ Pedro de Magalhaes~ Institute of Integrative Biology, University of Liverpool, Biosciences Building, Room 245, Crown Street, Liverpool, L69 7ZB, UK article info abstract Article history: Whether we are alone in the universe is one of the greatest mysteries facing humankind. Given the >100 Received 3 March 2016 billion stars in our galaxy, many have argued that it is statistically unlikely that life, including intelligent Accepted 16 June 2016 life, has not emerged anywhere else. The lack of any sign of extraterrestrial intelligence, even though on a Available online 26 July 2016 cosmic timescale extraterrestrial civilizations would have enough time to cross the galaxy, is known as Fermi's Paradox. One possible explanation for Fermi's Paradox is the Zoo Hypothesis which states that Keywords: one or more extraterrestrial civilizations know of our existence and can reach us, but have chosen not to Active SETI disturb us or even make their existence known to us. I propose here a proactive test of the Zoo Hy- Astrobiology fi Fermi's Paradox pothesis. Speci cally, I propose to send a message using television and radio channels to any extrater- Messaging to extraterrestrial intelligence restrial civilization(s) that might be listening and inviting them to respond. Even though I accept this is METI unlikely to be successful in the sense of resulting in a response from extraterrestrial intelligences, the possibility that extraterrestrial civilizations are monitoring us cannot be dismissed and my proposal is consistent with current scientific knowledge. -
Fine-Structure Feii and Siii Absorption in the Spectrum of GRB 051111
Draft version November 11, 2018 Preprint typeset using LATEX style emulateapj Fine-Structure Fe II and Si II Absorption in the Spectrum of GRB051111: Implications for the Burst Environment E. Berger1,2,3, B. E. Penprase4, D. B. Fox5, S. R. Kulkarni6, G. Hill7, B. Schaefer7, and M. Reed7 Draft version November 11, 2018 ABSTRACT We present an analysis of fine-structure transitions of Fe II and Si II detected in a high-resolution optical spectrum of the afterglow of GRB051111 (z =1.54948). The fine-structure absorption features arising from Fe II* to Fe II****, as well as Si II*, are confined to a narrow velocity structure extending over ±30 km s−1, which we interpret as the burst local environment, most likely a star forming region. We investigate two scenarios for the excitation of the fine-structure levels by collisions with electrons and radiative pumping by an infra-red or ultra-violet radiation field produced by intense star formation in the GRB environment, or by the GRB afterglow itself. We find that the conditions required for collisional excitation of Fe II fine-structure states cannot be easily reconciled with the relatively weak Si II* absorption. Radiative pumping by either IR or UV emission requires > 103 massive hot OB stars within a compact star-forming region a few pc in size, and in the case of IR pumping a large dust content. On the other hand, it is possible that the GRB itself provides the source of IR and/or UV radiation, in which case we estimate that the excitation takes place at a distance of ∼ 10 − 20 pc from the burst. -
Eclipsing Systems with Pulsating Components (Types Β Cep, Δ Sct, Γ Dor Or Red Giant) in the Era of High-Accuracy Space Data
galaxies Review Eclipsing Systems with Pulsating Components (Types b Cep, d Sct, g Dor or Red Giant) in the Era of High-Accuracy Space Data Patricia Lampens Royal Observatory of Belgium, Ringlaan 3, 1180 Brussels, Belgium; [email protected] Abstract: Eclipsing systems are essential objects for understanding the properties of stars and stellar systems. Eclipsing systems with pulsating components are furthermore advantageous because they provide accurate constraints on the component properties, as well as a complementary method for pulsation mode determination, crucial for precise asteroseismology. The outcome of space missions aiming at delivering high-accuracy light curves for many thousands of stars in search of planetary systems has also generated new insights in the field of variable stars and revived the interest of binary systems in general. The detection of eclipsing systems with pulsating components has particularly benefitted from this, and progress in this field is growing fast. In this review, we showcase some of the recent results obtained from studies of eclipsing systems with pulsating components based on data acquired by the space missions Kepler or TESS. We consider different system configurations including semi-detached eclipsing binaries in (near-)circular orbits, a (near-)circular and non-synchronized eclipsing binary with a chemically peculiar component, eclipsing binaries showing the heartbeat phenomenon, as well as detached, eccentric double-lined systems. All display one or more pulsating component(s). Among the great variety of known classes of pulsating stars, we discuss unevolved or slightly evolved pulsators of spectral type B, A or F and red giants with solar-like oscillations. Some systems exhibit additional phenomena such as tidal effects, angular momentum transfer, (occasional) Citation: Lampens, P. -
International Astronomical Union Commission G1 BIBLIOGRAPHY
International Astronomical Union Commission G1 BIBLIOGRAPHY OF CLOSE BINARIES No. 108 Editor-in-Chief: W. Van Hamme Editors: R.H. Barb´a D.R. Faulkner P.G. Niarchos D. Nogami R.G. Samec C.D. Scarfe C.A. Tout M. Wolf M. Zejda Material published by March 15, 2019 BCB issues are available at the following URLs: http://ad.usno.navy.mil/wds/bsl/G1_bcb_page.html, http://faculty.fiu.edu/~vanhamme/IAU-BCB/. The bibliographical entries for Individual Stars and Collections of Data, as well as a few General entries, are categorized according to the following coding scheme. Data from archives or databases, or previously published, are identified with an asterisk. The observation codes in the first four groups may be followed by one of the following wavelength codes. g. γ-ray. i. infrared. m. microwave. o. optical r. radio u. ultraviolet x. x-ray 1. Photometric data a. CCD b. Photoelectric c. Photographic d. Visual 2. Spectroscopic data a. Radial velocities b. Spectral classification c. Line identification d. Spectrophotometry 3. Polarimetry a. Broad-band b. Spectropolarimetry 4. Astrometry a. Positions and proper motions b. Relative positions only c. Interferometry 5. Derived results a. Times of minima b. New or improved ephemeris, period variations c. Parameters derivable from light curves d. Elements derivable from velocity curves e. Absolute dimensions, masses f. Apsidal motion and structure constants g. Physical properties of stellar atmospheres h. Chemical abundances i. Accretion disks and accretion phenomena j. Mass loss and mass exchange k. Rotational velocities 6. Catalogues, discoveries, charts a. Catalogues b. Discoveries of new binaries and novae c. -
Searching for SETI: the Social Construction of Aliens and the Quest for a Technological Mythos
Searching for SETI: The Social Construction of Aliens and the Quest for a Technological Mythos John Marvin Bozeman Dissertation submitted to the faculty of the Virginia Polytechnic Institute and State University in partial fulfillment of the requirements for the degree of Doctor of Philosophy In Science and Technology Studies Janet A. Abbate, Co-Chair Shannon A. Brown, Co-Chair Lee L. Zwanziger Paul D. Renard March 24, 2015 Falls Church, Virginia Keywords: Search for Extraterrestrial Intelligence, SETI, Actor Network Theory, Social Construction of Technology, Rational Choice Theory of Religion, Transhumanism, Xenosalvation Copyright John M. Bozeman Searching for SETI: The Social Construction of Aliens and the Quest for a Technological Mythos John M. Bozeman ABSTRACT This dissertation uses Actor Network Theory (ANT) and Stark and Bainbridge’s rational choice theory of religion to analyze an established but controversial branch of science and technology, the Search for Extraterrestrial Intelligence (SETI). Of particular interest are the cultural, and sometimes religious, assumptions that its creators have built into it. The purpose of this analysis is not to discredit SETI, but instead to show how SETI, along with other avant-garde scientific projects, is founded, motivated, and propelled by many of the same types of values and visions for the future that motivate the founders of religious groups. I further argue that the utopian zeal found in SETI and similar movements is not aberrant, but instead common, and perhaps necessary, in many early- stage projects, whether technical or spiritual, which lack a clear near-term commercial or social benefit. DEDICATION In memory of my parents, James E. -
Macrocosmo Nº33
HA MAIS DE DOIS ANOS DIFUNDINDO A ASTRONOMIA EM LÍNGUA PORTUGUESA K Y . v HE iniacroCOsmo.com SN 1808-0731 Ano III - Edição n° 33 - Agosto de 2006 * t i •■•'• bSÈlÈWW-'^Sif J fé . ’ ' w s » ws» ■ ' v> í- < • , -N V Í ’\ * ' "fc i 1 7 í l ! - 4 'T\ i V ■ }'- ■t i' ' % r ! ■ 7 ji; ■ 'Í t, ■ ,T $ -f . 3 j i A 'A ! : 1 l 4/ í o dia que o ceu explodiu! t \ Constelação de Andrômeda - Parte II Desnudando a princesa acorrentada £ Dicas Digitais: Softwares e afins, ATM, cursos online e publicações eletrônicas revista macroCOSMO .com Ano III - Edição n° 33 - Agosto de I2006 Editorial Além da órbita de Marte está o cinturão de asteróides, uma região povoada com Redação o material que restou da formação do Sistema Solar. Longe de serem chamados como simples pedras espaciais, os asteróides são objetos rochosos e/ou metálicos, [email protected] sem atmosfera, que estão em órbita do Sol, mas são pequenos demais para serem considerados como planetas. Até agora já foram descobertos mais de 70 Diretor Editor Chefe mil asteróides, a maior parte situados no cinturão de asteróides entre as órbitas Hemerson Brandão de Marte e Júpiter. [email protected] Além desse cinturão podemos encontrar pequenos grupos de asteróides isolados chamados de Troianos que compartilham a mesma órbita de Júpiter. Existem Editora Científica também aqueles que possuem órbitas livres, como é o caso de Hidalgo, Apolo e Walkiria Schulz Ícaro. [email protected] Quando um desses asteróides cruza a nossa órbita temos as crateras de impacto. A maior cratera visível de nosso planeta é a Meteor Crater, com cerca de 1 km de Diagramadores diâmetro e 600 metros de profundidade. -
Hydrogen Subordinate Line Emission at the Epoch of Cosmological Recombination M
Astronomy Reports, Vol. 47, No. 9, 2003, pp. 709–716. Translated from Astronomicheski˘ı Zhurnal, Vol. 80, No. 9, 2003, pp. 771–779. Original Russian Text Copyright c 2003 by Burgin. Hydrogen Subordinate Line Emission at the Epoch of Cosmological Recombination M. S. Burgin Astro Space Center, Lebedev Physical Institute, Russian Academy of Sciences, Profsoyuznaya ul. 84/32, Moscow, 117997 Russia Received December 10, 2002; in final form, March 14, 2003 Abstract—The balance equations for the quasi-stationary recombination of hydrogen plasma in a black- body radiation field are solved. The deviations of the excited level populations from equilibrium are computed and the rates of uncompensated line transitions determined. The expressions obtained are stable for computations of arbitrarily small deviations from equilibrium. The average number of photons emitted in hydrogen lines per irreversible recombination is computed for plasma parameters corresponding to the epoch of cosmological recombination. c 2003 MAIK “Nauka/Interperiodica”. 1. INTRODUCTION of this decay is responsible for the appreciable differ- When the cosmological expansion of the Universe ence between the actual degree of ionization and the lowered the temperature sufficiently, the initially ion- value correspondingto the Saha –Boltzmann equi- ized hydrogen recombined. According to [1, 2], an librium. A detailed analysis of processes affectingthe appreciable fraction of the photons emitted at that recombination rate and computations of the temporal time in subordinate lines survive to the present, lead- behavior of the degree of ionization for various sce- ingto the appearance of spectral lines in the cosmic narios for the cosmological expansion are presented background (relict) radiation. Measurements of the in [5, 6]. -
The Atmospheric Parameters and Spectral Interpolator for the MILES Stars
A&A 531, A165 (2011) Astronomy DOI: 10.1051/0004-6361/201116769 & c ESO 2011 Astrophysics The atmospheric parameters and spectral interpolator for the MILES stars Ph. Prugniel1, I. Vauglin1,andM.Koleva2,1 1 Université de Lyon, Université Lyon 1, 69622 Villeurbanne, France; CRAL, Observatoire de Lyon, CNRS UMR 5574, 69561 Saint-Genis Laval, France e-mail: [philippe.prugniel;isabelle.vauglin]@univ-lyon1.fr 2 Instituto de Astrofísica de Canarias, La Laguna, 38200 Tenerife, Spain; Departamento de Astrofísica, Universidad de La Laguna, 38205 La Laguna, Tenerife, Spain e-mail: [email protected] Received 22 February 2011 / Accepted 16 April 2011 ABSTRACT Context. Empirical libraries of stellar spectra are used to classify stars and synthetize stellar populations. MILES is a medium spectral- resolution library in the optical domain covering a wide range of temperatures, surface gravities and metallicities. Aims. We redetermine the atmospheric parameters of these stars in order to improve the homogeneity and accuracy. We build an interpolating function that returns a spectrum as a function of the three atmospheric parameters, and finally we characterize the precision of the wavelength calibration and stability of the spectral resolution. Methods. We used the ULySS program with the ELODIE library as a reference and compared the results with those in the literature. Results. We obtain precisions of 60 K, 0.13, and 0.05 dex, respectively, for Teff ,logg,and[Fe/H] for the FGK stars. For the M stars, the mean errors are 38 K, 0.26, and 0.12 dex and 3.5%, 0.17, and 0.13 dex for the OBA. -
Communication with Extraterrestrial Intelligence Through Radio Signals and Messages 1A
ISSN : 2230-7109 (Online) | ISSN : 2230-9543 (Print) IJECT VOL . 5, ISSU E SPL - 2, JAN - MAR C H 2014 Communication with Extraterrestrial Intelligence Through Radio Signals and Messages 1A. B. Bhattacharya, 2A. Sarkar 1,2Dept. of Physics, University of Kalyani, Kalyani, WB, India Abstract hundred yards wide could delineate twenty-mile wide shapes and The paper summarizes the present day research knowledge based then the trenches would be filled with water after which enough on communication with extraterrestrial intelligence through four kerosene could be poured on top of the water to burn for six hours. distinct means covering mathematical languages, pictorial systems Using this technique, a different signal could be sent every night. like the Arecibo message, algorithmic communication systems and In the mean time other astronomers were looking for signs of life computational approaches for detecting and deciphering ‘natural’ on other planets. In 1822, Franz von Gruithuisen [Cattermole and language communication. Moore, 1997] imagined a giant city and evidence of agriculture on the moon and believed evidence of life on Venus but astronomers Keywords using more sophisticated instruments refuted his claims. By the Arecibo Message, Communication, Extraterrestrial Intelligence, late 1800s, Astronomers believed the Kant-Laplace hypothesis, Resonant Receiver which stated that the farthest planets from the sun are the oldest and so Mars was more likely to have advanced civilizations than I. Introduction Venus. Subsequent investigations focused on contacting Martians. Communication with Extraterrestrial Intelligence (CETI) is Charles Cros [Ley, 1958] was convinced that pinpoints of light a subject matter under the SETI (Search for Extraterrestrial observed on Mars and Venus were the lights of large cities and Intelligence) research which focuses on composing and was attempted to get funding for a giant mirror with which to deciphering messages that could be understood theoretically signal the Martians. -
Extrasolar Planet Detection and Characterization with the KELT-North Transit Survey
Extrasolar Planet Detection and Characterization With the KELT-North Transit Survey DISSERTATION Presented in Partial Fulfillment of the Requirements for the Degree Doctor of Philosophy in the Graduate School of The Ohio State University By Thomas G. Beatty Graduate Program in Astronomy The Ohio State University 2014 Dissertation Committee: Professor B. Scott Gaudi, Advisor Professor Andrew P. Gould Professor Marc H. Pinsonneault Copyright by Thomas G. Beatty 2014 Abstract My dissertation focuses on the detection and characterization of new transiting extrasolar planets from the KELT-North survey, along with a examination of the processes underlying the astrophysical errors in the type of radial velocity measurements necessary to measure exoplanetary masses. Since 2006, the KELT- North transit survey has been collecting wide-angle precision photometry for 20% of the sky using a set of target selection, lightcurve processing, and candidate identification protocols I developed over the winter of 2010-2011. Since our initial set of planet candidates were generated in April 2011, KELT-North has discovered seven new transiting planets, two of which are among the five brightest transiting hot Jupiter systems discovered via a ground-based photometric survey. This highlights one of the main goals of the KELT-North survey: to discover new transiting systems orbiting bright, V< 10, host stars. These systems offer us the best targets for the precision ground- and space-based follow-up observations necessary to measure exoplanetary atmospheres. In September 2012 I demonstrated the atmospheric science enabled by the new KELT planets by observing the secondary eclipses of the brown dwarf KELT-1b with the Spitzer Space Telescope. -
A Profile of Humanity: the Cultural Signature of Earth's Inhabitants
International Journal of A profile of humanity: the cultural signature of Astrobiology Earth’s inhabitants beyond the atmosphere cambridge.org/ija Paul E. Quast Beyond the Earth foundation, Edinburgh, UK Research Article Abstract Cite this article: Quast PE (2018). A profile of The eclectic range of artefacts and ‘messages’ we dispatch into the vast expanse of space may humanity: the cultural signature of Earth’s become one of the most enduring remnants of our present civilization, but how does his pro- inhabitants beyond the atmosphere. tracted legacy adequately document the plurality of societal values and common, cultural heri- International Journal of Astrobiology 1–21. https://doi.org/10.1017/S1473550418000290 tage on our heterogeneous world? For decades now, this rendition of the egalitarian principle has been explored by the Search for Extra-Terrestrial Intelligence community in order to draft Received: 18 April 2018 theoretical responses to ‘who speaks for Earth?’ for hypothetical extra-terrestrial communica- Revised: 13 June 2018 tion strategies. However, besides the moral, ethical and democratic advancements made by Accepted: 21 June 2018 this particular enterprise, there remains little practical exemplars of implementing this gar- Key words: nered knowledge into other experimental elements that could function as mutual emissaries Active SETI; data storage; deep time messages; of Earth; physical artefacts that could provide accessible details about our present world for eternal memory archives; future archaeology; future archaeological observations by our space-faring progeny, potential visiting extrasolar long-term communication strategies; SETI; time capsules denizens or even for posterity. While some initiatives have been founded to investigate this enduring dilemma of humanity over the last half-century, there are very few comparative stud- Author for correspondence: ies in regards to how these objects, time capsules and transmission events collectively dissem- Paul E. -
Vol 11 No 2, Spring 2005
SearchLites Vol. 11 No. 2, Spring 2005 The Quarterly Newsletter of The SETI League, Inc. Offices: 433 Liberty Street Scaling Back on SETICon PO Box 555 Little Ferry NJ Little Ferry, NJ.., 19 February 2005 -- Five years after initiating its SETICon Technical 07643 USA Symposium, the nonprofit, membership-supported SETI League has had to scale back the annual membership event to more modest proportions. Because The SETI League chose Phone: to make its meetings affordable and accessible to a wide range of amateur radio astrono- (201) 641-1770 Facsimile: mers, the events have proved a steady drain on the grassroots science group's limited fi- (201) 641-1771 nancial resources. Hence, the organization's 2005 annual meeting will be held in conjunc- Email: tion with another, much larger and well-established conference. [email protected] Web: "The last few SETICons cost us about $4,000 each to put on," notes Dr. H. Paul www.setileague.org Shuch, volunteer executive director of The SETI League. "Depending as we do upon President: membership dues and individual contributions, we thought our limited funding would be Richard Factor better spent on SETI science than on hosting scientific meetings." Consequently, Shuch Registered Agent: announced, The SETI League's 2005 Annual Membership Meeting will be held on the Marc Arnold, Esq. campus of The College of New Jersey, in conjunction with the annual Trenton Computer Secretary/Treasurer: A. Heather Wood Festival. Executive Director: H. Paul Shuch, Ph.D. This year's Trenton Computer Festival is scheduled to run the weekend of 16-17 April, 2005, with The SETI League's membership meeting to be held there on Sunday morning, 17 April, from 10 AM until Noon.