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Henryk Siemiradzki and the International Artistic Milieu
ACCADEMIA POL ACCA DELLE SCIENZE DELLE SCIENZE POL ACCA ACCADEMIA BIBLIOTECA E CENTRO DI STUDI A ROMA E CENTRO BIBLIOTECA ACCADEMIA POLACCA DELLE SCIENZE BIBLIOTECA E CENTRO DI STUDI A ROMA CONFERENZE 145 HENRYK SIEMIRADZKI AND THE INTERNATIONAL ARTISTIC MILIEU FRANCESCO TOMMASINI, L’ITALIA E LA RINASCITA E LA RINASCITA L’ITALIA TOMMASINI, FRANCESCO IN ROME DELLA INDIPENDENTE POLONIA A CURA DI MARIA NITKA AGNIESZKA KLUCZEWSKA-WÓJCIK CONFERENZE 145 ACCADEMIA POLACCA DELLE SCIENZE BIBLIOTECA E CENTRO DI STUDI A ROMA ISSN 0239-8605 ROMA 2020 ISBN 978-83-956575-5-9 CONFERENZE 145 HENRYK SIEMIRADZKI AND THE INTERNATIONAL ARTISTIC MILIEU IN ROME ACCADEMIA POLACCA DELLE SCIENZE BIBLIOTECA E CENTRO DI STUDI A ROMA CONFERENZE 145 HENRYK SIEMIRADZKI AND THE INTERNATIONAL ARTISTIC MILIEU IN ROME A CURA DI MARIA NITKA AGNIESZKA KLUCZEWSKA-WÓJCIK. ROMA 2020 Pubblicato da AccademiaPolacca delle Scienze Bibliotecae Centro di Studi aRoma vicolo Doria, 2 (Palazzo Doria) 00187 Roma tel. +39 066792170 e-mail: [email protected] www.rzym.pan.pl Il convegno ideato dal Polish Institute of World Art Studies (Polski Instytut Studiów nad Sztuką Świata) nell’ambito del programma del Ministero della Scienza e dell’Istruzione Superiore della Repubblica di Polonia (Polish Ministry of Science and Higher Education) “Narodowy Program Rozwoju Humanistyki” (National Programme for the Develop- ment of Humanities) - “Henryk Siemiradzki: Catalogue Raisonné of the Paintings” (“Tradition 1 a”, no. 0504/ nprh4/h1a/83/2015). Il convegno è stato organizzato con il supporto ed il contributo del National Institute of Polish Cultural Heritage POLONIKA (Narodowy Instytut Polskiego Dziedzictwa Kul- turowego za Granicą POLONIKA). Redazione: Maria Nitka, Agnieszka Kluczewska-Wójcik Recensione: Prof. -
Meteor Shower Detection with Density-Based Clustering
Meteor Shower Detection with Density-Based Clustering Glenn Sugar1*, Althea Moorhead2, Peter Brown3, and William Cooke2 1Department of Aeronautics and Astronautics, Stanford University, Stanford, CA 94305 2NASA Meteoroid Environment Office, Marshall Space Flight Center, Huntsville, AL, 35812 3Department of Physics and Astronomy, The University of Western Ontario, London N6A3K7, Canada *Corresponding author, E-mail: [email protected] Abstract We present a new method to detect meteor showers using the Density-Based Spatial Clustering of Applications with Noise algorithm (DBSCAN; Ester et al. 1996). DBSCAN is a modern cluster detection algorithm that is well suited to the problem of extracting meteor showers from all-sky camera data because of its ability to efficiently extract clusters of different shapes and sizes from large datasets. We apply this shower detection algorithm on a dataset that contains 25,885 meteor trajectories and orbits obtained from the NASA All-Sky Fireball Network and the Southern Ontario Meteor Network (SOMN). Using a distance metric based on solar longitude, geocentric velocity, and Sun-centered ecliptic radiant, we find 25 strong cluster detections and 6 weak detections in the data, all of which are good matches to known showers. We include measurement errors in our analysis to quantify the reliability of cluster occurrence and the probability that each meteor belongs to a given cluster. We validate our method through false positive/negative analysis and with a comparison to an established shower detection algorithm. 1. Introduction A meteor shower and its stream is implicitly defined to be a group of meteoroids moving in similar orbits sharing a common parentage. -
Solar Writer Report for Abraham Lincoln
FIXED STARS A Solar Writer Report for Abraham Lincoln Written by Diana K Rosenberg Compliments of:- Stephanie Johnson Seeing With Stars Astrology PO Box 159 Stepney SA 5069 Australia Tel/Fax: +61 (08) 8331 3057 Email: [email protected] Web: www.esotech.com.au Page 2 Abraham Lincoln Natal Chart 12 Feb 1809 12:40:56 PM UT +0:00 near Hodgenville 37°N35' 085°W45' Tropical Placidus 22' 13° 08°ˆ ‡ 17' ¾ 06' À ¿É ‰ 03° ¼ 09° 00° 06° 09°06° ˆ ˆ ‡ † ‡ 25° 16' 41'08' 40' † 01' 09' Œ 29' ‰ 9 10 23° ¶ 8 27°‰ 11 Ï 27° 01' ‘ ‰02' á 7 12 ‘ áá 23° á 23° ¸ 23°Š27' á Š à „ 28' 28' 6 18' 1 10°‹ º ‹37' 13° 05' ‹ 5 Á 22° ½ 27' 2 4 01' Ü 3 07° Œ ƒ » 09' 23° 09° Ý Ü 06° 16' 06' Ê 00°ƒ 13° 22' Ý 17' 08°‚ Page 23 Astrological Summary Chart Point Positions: Abraham Lincoln Planet Sign Position House Comment The Moon Capricorn 27°Cp01' 12th The Sun Aquarius 23°Aq27' 12th read into 1st House Mercury Pisces 10°Pi18' 1st Venus Aries 7°Ar27' 1st read into 2nd House Mars Libra 25°Li29' 8th Jupiter Pisces 22°Pi05' 1st Saturn Sagittarius 3°Sg08' 9th read into 10th House Uranus Scorpio 9°Sc40' 8th Neptune Sagittarius 6°Sg41' 9th read into 10th House Pluto Pisces 13°Pi37' 1st The North Node Scorpio 6°Sc09' 8th The South Node Taurus 6°Ta09' 2nd The Ascendant Aquarius 23°Aq28' 1st The Midheaven Sagittarius 8°Sg22' 10th The Part of Fortune Capricorn 27°Cp02' 12th Chart Point Aspects Planet Aspect Planet Orb App/Sep The Moon Square Mars 1°32' Separating The Moon Conjunction The Part of Fortune 0°00' Applying The Sun Trine Mars 2°02' Applying The Sun Conjunction The Ascendant -
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. -
The Young Active Binary Star EK Draconis
A&A 435, 215–223 (2005) Astronomy DOI: 10.1051/0004-6361:20040462 & c ESO 2005 Astrophysics The young active binary star EK Draconis B. König1,2,E.W.Guenther3, J. Woitas3, and A. P. Hatzes3 1 Max-Planck-Institut für extraterrestrische Physik, Gießenbachstraße 1, 85748 Garching, Germany 2 University of Pittsburgh, 3941 O’Hara St, Pittsburgh, PA 15260, USA e-mail: [email protected] 3 Thüringer Landessternwarte Tautenburg, Sternwarte 5, 07778 Tautenburg, Germany Received 17 March 2004 / Accepted 18 January 2005 Abstract. EK Dra (HD 129333) is a young, active, nearby star that is orbited by a low mass companion. By combining new speckle observations with old and new radial velocity measurements we find that the orbit is highly eccentric with e = 0.82 ± 0.03, and we derive the true masses of both components. The masses are 0.9 ± 0.1 M and 0.5 ± 0.1 M, for the primary and secondary, respectively. From high resolution spectra we derive a new Teff of 5700 ± 70 K and a log g of 4.37 ± 0.10, which is different to previous estimates. However, the new spectroscopic distance differs by only 5.8% to the distance derived by parallax measurement by the Hipparcos satellite and thus the stellar parameters are presumably more realistic than older determinations. We derive a somewhat higher value for the metallicity of [Fe/H] = −0.16 ± 0.07. EK Dra turns out to be one of the few nearby young stars that will evolve similarly to the Sun. The precise radial velocity measurements taken in the course of this program also allow us to shed more light on the activity of this star. -
Tabetha Boyajian's CV
Dr. Tabetha Boyajian Yale University, Department of Astronomy, 52 Hillhouse Ave., New Haven, CT 06520 USA [email protected] • +1 (404) 849-4848 • http://www.astro.yale.edu/tabetha PROFESSIONAL Yale University, Department of Astronomy, New Haven, Connecticut, USA EXPERIENCE Postdoctoral Fellow 2012 – present • Supervisor: Dr. Debra Fischer Center for high Angular Resolution Astronomy (CHARA), Georgia State University Hubble Fellow 2009 – 2012 • Supervisor: Dr. Harold McAlister EDUCATION Georgia State University, Department of Physics and Astronomy, Atlanta, Georgia, USA Doctor of Philosophy (Ph.D.) in Astronomy 2005 – 2009 • Adviser: Dr. Harold McAlister Master of Science (M.S.) in Physics 2003 – 2005 • Adviser: Dr. Douglas Gies College of Charleston, Charleston, South Carolina, USA Bachelor of Science (B.S.) in Physics with concentration in astronomy 1998 – 2003 • Graduated with Departmental Honors PROFESSIONAL Secretary, International Astronomical Union, Division G 2015 – 2018 SERVICE Steering Committee, International Astronomical Union, Division G 2015 – 2018 Review panel member NASA Kepler Guest Observer program, NASA K2 Guest Observer program, NSF-AAG program Referee The Astronomical Journal, Astronomy & Astrophysics, PASA Telescope time allocation committee member CHARA, OPTICON (external) AREAS OF Fundamental properties of stars: diameters, temperatures, exoplanet detection and characterization, SPECIALIZATION Optical/IR interferometry, stellar spectroscopy (radial velocities, abundances, activity), absolute AND INTEREST -
Download This Issue (Pdf)
Volume 46 Number 1 JAAVSO 2018 The Journal of the American Association of Variable Star Observers Optical Flares and Quasi-Periodic Pulsations on CR Draconis during Periastron Passage Upper panel: 2017-10-10-flare photon counts, time aligned with FFT spectrogram. Lower panel: FFT spectrogram shows time in UT seconds versus QPP periods in seconds. Flares cited by Doyle et al. (2018) are shown with (*). Also in this issue... • The Dwarf Nova SY Cancri and its Environs • KIC 8462852: Maria Mitchell Observatory Photographic Photometry 1922 to 1991 • Visual Times of Maxima for Short Period Pulsating Stars III • Recent Maxima of 86 Short Period Pulsating Stars Complete table of contents inside... The American Association of Variable Star Observers 49 Bay State Road, Cambridge, MA 02138, USA The Journal of the American Association of Variable Star Observers Editor John R. Percy Kosmas Gazeas Kristine Larsen Dunlap Institute of Astronomy University of Athens Department of Geological Sciences, and Astrophysics Athens, Greece Central Connecticut State University, and University of Toronto New Britain, Connecticut Toronto, Ontario, Canada Edward F. Guinan Villanova University Vanessa McBride Associate Editor Villanova, Pennsylvania IAU Office of Astronomy for Development; Elizabeth O. Waagen South African Astronomical Observatory; John B. Hearnshaw and University of Cape Town, South Africa Production Editor University of Canterbury Michael Saladyga Christchurch, New Zealand Ulisse Munari INAF/Astronomical Observatory Laszlo L. Kiss of Padua Editorial Board Konkoly Observatory Asiago, Italy Geoffrey C. Clayton Budapest, Hungary Louisiana State University Nikolaus Vogt Baton Rouge, Louisiana Katrien Kolenberg Universidad de Valparaiso Universities of Antwerp Valparaiso, Chile Zhibin Dai and of Leuven, Belgium Yunnan Observatories and Harvard-Smithsonian Center David B. -
2019 Destination Imagination Global Finals Escape Artists Results File:///C:/Users/Tinas/Desktop/GF19 Results/Tournamentresults-ESCAPE
2019 Destination Imagination Global Finals Escape Artists Results file:///C:/Users/tinas/Desktop/GF19 results/TournamentResults-ESCAPE... Destination Imagination congratulates all the students who participated in the Kansas City tournament. We think you are all winners! Teams emphasized as such are going on to the next level of competition. pO: Escape Artists, Elementary Level Total Central Choice Instant Rank Name Town Mbrshp# Deduct Rw. Cen Rw.TCE RwInst Tragic Magic, 359.07 240.00 60.00 59.07 1 Deerfield, Illinois 114-87177 Walden - DPS 109 0.00 198.53 52.28 53.75 Whitestone 1- 352.04 211.63 54.97 85.44 2 Quirky Queens, LEANDER ISD, Texas 750-63539 WHITESTONE EL 0.00 175.06 47.90 77.75 Superior 7, Zue 339.94 192.44 49.97 97.53 3 Bales Intermediate Friendswood ISD, Texas 750-05676 School 0.00 159.19 43.54 88.75 Chalk It Up!, 337.90 196.21 45.54 96.15 4 WYLIE ISD, Texas 750-27357 WYLIE INT 0.00 162.31 39.68 87.50 Creative Crayons, PFLUGERVILLE ISD, 326.94 208.27 49.99 68.68 5 750-77238 TIMMERMAN EL Texas 0.00 172.28 43.56 62.50 Service Ninjas, MIDLOTHIAN ISD, 323.01 209.34 55.70 57.97 6 750-31300 Miller Elementary Texas 0.00 173.17 48.53 52.75 Hurricane Helpers, 317.64 179.13 39.88 98.63 7 Terrace Park - 5th Terrace Park, Ohio 135-63707 grade Buchholz 0.00 148.18 34.75 89.75 The Spicy DI ritos, 315.12 216.97 45.40 52.75 8 KLEIN ISD, Texas 750-92814 METZLER EL 0.00 179.48 39.56 48.00 Fantastic 5, 313.69 193.77 39.70 80.22 9 Warren, Ohio 135-81882 Howland LSD 0.00 160.29 34.59 73.00 Screaming Main 310.36 176.29 36.82 97.25 Melody, Beijing 10 China 185-63578 Huilongguan YuXin 0.00 145.83 32.08 88.50 Sch of CNU 11T The Care Crew, St. -
1) the Case for Stochastic Orbital Migration 2) Open Exoplanet Catalogue
Institute for Advanced Study 1) The case for stochastic orbital migration 2) Open Exoplanet Catalogue Hanno Rein @ CITA, March 2013 Extra-solar planet census All discovered extra-solar planets 869 confirmed extra- solar planets • Super-Jupiters • (Hot) Jupiters • Neptunes • Super-Earths • Earth-like planets Open Exoplanet Catalogue (Rein 2012b) All multi-planetary systems 327 confirmed planets in multi-planetary systems • Multiple Jupiters • Densely packed systems of Neptunes and (Super)-Earths • 1 Solar System • Some systems are deep in resonance Open Exoplanet Catalogue (Rein 2012b) Radial velocity planets 80 RV planets 70 Cumulative period ] 60 ratio in multi- 10 jup [M planetary systems 2 50 + m 1 • Periods of systems with 40 massive planets tend to pile up near integer number of pairs 30 ratios 1 20 total planet mass m • Most prominent 10 features at 4:1, 3:1, 2:1, 0 3:2 1 1.33 1.5 2 3 4 5 6 7 8 9 period ratio 300 0.1 KOI planets 250 ] jup [M Rein, Payne, Veras & Ford (2012) 200 2 + m 1 150 number of pairs 100 total planet mass m 50 0 0.01 1 1.33 1.5 2 3 4 5 6 7 8 9 period ratio Kepler candidates 2740 planet candidates • Probing a different regime • Small mass planets • A lot of planets Open Exoplanet Catalogue (Rein 2012b) Kepler candidates with multiple planets Kepler multi-planetary systems • Small mass planets • Hierarchical systems • Densely packed • Not many are in resonance Open Exoplanet Catalogue (Rein 2012b) 80 RV planets 70 ] 60 10 jup [M 2 50 + m 1 40 number of pairs 30 1 20 total planet mass m Kepler's 10 transiting planet -
96P/Machholz
The age of the meteoroid complex of comet 96P/Machholz Abedin Y. Abedin Paul A. Wiegert Petr Pokorny Peter G. Brown Introduction • Associated with 8 meteor showers - QUA, ARI, SDA, NDA, KVE, Carinids, 훂-Cetids, Ursids. (Babadzhanov & Obrubov, 1992) • Previous age estimates – QUA, ARI, SDA, NDA => 2200 - 7000 years Jones & Jones (1993), Wu & Williams (1993), Neslusan et al. (2013) • Recently ARI, SDA, NDA associated with the Marsden group of comets – Ohtsuka et al. (2003), Sekanina & Chodas (2005), Jenniskens (2012) – ARI, SDA, NDA, along with Marsden group of comets, formed between 100 AD – 900 AD Our work • Simulations of stream formation. – 96P/Machholz => 20000 BC – Marsden group (P/1999 J6) => 100 AD • We find by simultaneously fitting shower profiles, radiant and orbital elements that: 1. We find that 96P contributes to all 8 showers, whereas P/1999 J6 to only 3. 2. Marsden group of comets alone can not explain the observed duration of the showers. 3. The complex is much older that previously suggested Results from simulations Showers of 96P/Machholz Showers of P/1999 J6 Meteoroid ejection 20000 BC Meteoroid ejection onset 100 AD QUA NID ARI NDA ARI SDA DLT SDA KVE TCA KVE 90 <-- 0 <-- 270 <--180 <-- 90 90 <-- 0 <-- 270 <--180 <-- 90 Southern Delta Aquariids (SDA) Age: 100 AD Parent body: Marsden group of comets (P/1999 J6) Sekanina & Chodas (2005) Ejection epoch Residuals Grey – observations Red - Simulations SDA – Continued Meteoroid Ejection onset time: 20000 BC Assumed parent body: 96P/Machholz Ejection epoch Residuals Grey – observations Red - Simulations SDA – Combined profile Marsden group (P/1999 J6) => 100 AD 96P/Machholz => 20000 BC Ejection epoch Residuals Grey – observations Red - Simulations SDA – radiant drift and position SDA Daytime Lambda Taurids Origin from comet 96P/Machholz => 20000 BC Ejection epoch Residuals Grey – observations Red - Simulations Radiant drift Daytime Lambda Taurids Radiant position DLT Cont. -
Confirmation of the Northern Delta Aquariids
WGN, the Journal of the IMO XX:X (200X) 1 Confirmation of the Northern Delta Aquariids (NDA, IAU #26) and the Northern June Aquilids (NZC, IAU #164) David Holman1 and Peter Jenniskens2 This paper resolves confusion surrounding the Northern Delta Aquariids (NDA, IAU #26). Low-light level video observations with the Cameras for All-sky Meteor Surveillance project in California show distinct showers in the months of July and August. The July shower is identified as the Northern June Aquilids (NZC, IAU #164), while the August shower matches most closely prior data on the Northern Delta Aquariids. This paper validates the existence of both showers, which can now be moved to the list of established showers. The August Beta Piscids (BPI, #342) is not a separate stream, but identical to the Northern Delta Aquariids, and should be discarded from the IAU Working List. We detected the Northern June Aquilids beginning on June 14, through its peak on July 11, and to the shower's end on August 2. The meteors move in a short-period sun grazing comet orbit. Our mean orbital elements are: q = 0:124 0:002 AU, 1=a = 0:512 0:014 AU−1, i = 37:63◦ 0:35◦, ! = 324:90◦ 0:27◦, and Ω = 107:93 0:91◦ (N = 131). This orbit is similar to that of sungrazer comet C/2009 U10. ◦ ◦ 346.4 , Decl = +1.4 , vg = 38.3 km/s, active from so- lar longitude 128.8◦ to 151.17◦. This position, however, 1 Introduction is the same as that of photographed Northern Delta Aquariids. -
The Electric Sun Hypothesis
Basics of astrophysics revisited. II. Mass- luminosity- rotation relation for F, A, B, O and WR class stars Edgars Alksnis [email protected] Small volume statistics show, that luminosity of bright stars is proportional to their angular momentums of rotation when certain relation between stellar mass and stellar rotation speed is reached. Cause should be outside of standard stellar model. Concept allows strengthen hypotheses of 1) fast rotation of Wolf-Rayet stars and 2) low mass central black hole of the Milky Way. Keywords: mass-luminosity relation, stellar rotation, Wolf-Rayet stars, stellar angular momentum, Sagittarius A* mass, Sagittarius A* luminosity. In previous work (Alksnis, 2017) we have shown, that in slow rotating stars stellar luminosity is proportional to spin angular momentum of the star. This allows us to see, that there in fact are no stars outside of “main sequence” within stellar classes G, K and M. METHOD We have analyzed possible connection between stellar luminosity and stellar angular momentum in samples of most known F, A, B, O and WR class stars (tables 1-5). Stellar equatorial rotation speed (vsini) was used as main parameter of stellar rotation when possible. Several diverse data for one star were averaged. Zero stellar rotation speed was considered as an error and corresponding star has been not included in sample. RESULTS 2 F class star Relative Relative Luminosity, Relative M*R *eq mass, M radius, L rotation, L R eq HATP-6 1.29 1.46 3.55 2.950 2.28 α UMi B 1.39 1.38 3.90 38.573 26.18 Alpha Fornacis 1.33