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Princeton University Library September 27, 2013
Checklist of Western Medieval, Byzantine, and Renaissance Manuscripts in the Princeton University Library and the Scheide Library Princeton University Library September 27, 2013 Contents Introduction, p. 3 Manuscripts Division Robert Garrett Medieval and Renaissance Manuscripts, p. 5 Robert Taylor Medieval and Renaissance Manuscripts, p. 44 Grenville Kane Medieval and Renaissance Manuscripts, p. 48 Princeton Medieval and Renaissance Manuscripts, p. 56 Cotsen Children’s Library Cotsen Medieval and Renaissance Manuscripts, p. 87 Rare Books Division Manuscripts bound with early printed books, p. 88 The Scheide Library Scheide Medieval and Renaissance Manuscripts, p. 88 Introduction The present checklist is not a catalogue, but rather is a checklist intended to serve as a guide to sources of up-to-date cataloging, textual and codicological description, and digital images for western medieval, Byzantine, and Renaissance manuscripts in the Princeton University Library and the Scheide Library. Manuscripts are listed by holding unit, collection, and manuscript number or shelfmark. Links are given for more than well over 2,000 digital images of miniatures, illustrations, and selected diagrams and decoration in the manuscripts, about a third of which are illuminated. In addition, links are provided for digitized grayscale microfilm of a large number of Middle English manuscripts at Princeton and for a group of important manuscripts digitized in the Library since the 1990s. For additional information about the holdings of the Manuscripts Division and to make appointments, potential researchers should contact Don C. Skemer, Curator of Manuscripts, at [email protected]. For information about holdings of the Scheide Library, please contact Paul Needham, Librarian, at [email protected] For information concerning photoduplication and permission to publish and/or broadcast, please send an email to [email protected] A brief overview of the manuscripts and their cataloging follows. -
Mars Mars Is the Fourth Terrestrial Planet. It Is Smaller in Size Than
Mars Mars is the fourth terrestrial planet. It is smaller in size than Earth and Venus, but larger than Mercury. Of the planets, Mars is the most hospitable to visiting humans, as it has an atmosphere, though it has no oxygen and is very thin. In the early days of the solar system, Mars has had liquid water on its surface, which is proved by the existence of various minerals that require liquid water to form. The current atmosphere of Mars is too thin and cold for liquid water to exist for long periods of times. Still, there is evidence of terrain shaped by flowing liquids, which are probably temporary flows or floods caused by the melting of ice in the ground. Mars has seasons like the Earth, and ice caps at the poles that grow and shrink over the course of the year. They consist of water ice and CO2 ice, the latter varying more with the seasons. One year on Mars is a bit less than two Earth years. Mars has two moons, Phobos and Deimos. They are very small compared to Mars, and are likely to be asteroids captured by Mars's gravity in the distant past. Giant planets and their moons The outer four planets of the solar system are known as the giant planets, because of their large size (compared to the terrestrial planets). The giant planets of our solar system can be further divided into two categories: gas giants (Jupiter and Saturn) and ice giants (Uranus and Neptune). The gas giants consist mainly of hydrogen (up to 90%) and helium, while the ice giants are mostly "ices" such as water and ammonia, with only some 20% of hydrogen. -
Comparative Habitability of Transiting Exoplanets
Draft version October 1, 2015 A Preprint typeset using LTEX style emulateapj v. 04/17/13 COMPARATIVE HABITABILITY OF TRANSITING EXOPLANETS Rory Barnes1,2,3, Victoria S. Meadows1,2, Nicole Evans1,2 Draft version October 1, 2015 ABSTRACT Exoplanet habitability is traditionally assessed by comparing a planet’s semi-major axis to the location of its host star’s “habitable zone,” the shell around a star for which Earth-like planets can possess liquid surface water. The Kepler space telescope has discovered numerous planet candidates near the habitable zone, and many more are expected from missions such as K2, TESS and PLATO. These candidates often require significant follow-up observations for validation, so prioritizing planets for habitability from transit data has become an important aspect of the search for life in the universe. We propose a method to compare transiting planets for their potential to support life based on transit data, stellar properties and previously reported limits on planetary emitted flux. For a planet in radiative equilibrium, the emitted flux increases with eccentricity, but decreases with albedo. As these parameters are often unconstrained, there is an “eccentricity-albedo degeneracy” for the habitability of transiting exoplanets. Our method mitigates this degeneracy, includes a penalty for large-radius planets, uses terrestrial mass-radius relationships, and, when available, constraints on eccentricity to compute a number we call the “habitability index for transiting exoplanets” that represents the relative probability that an exoplanet could support liquid surface water. We calculate it for Kepler Objects of Interest and find that planets that receive between 60–90% of the Earth’s incident radiation, assuming circular orbits, are most likely to be habitable. -
Dynamical Evolution and Bombardment of the Early Solar System: a Few Highlights from the Last 50 Years
50th Lunar and Planetary Science Conference 2019 (LPI Contrib. No. 2132) 1545.pdf DYNAMICAL EVOLUTION AND BOMBARDMENT OF THE EARLY SOLAR SYSTEM: A FEW HIGHLIGHTS FROM THE LAST 50 YEARS. W. F. Bottke1 1Southwest Research Institute and NASA’s SSERVI-ISET Team, Boulder, CO ([email protected]). Introduction. Over the last several decades, there orbital migration of Jupiter and Saturn in a gas disk, has been a transformation in our theoretical under- Jupiter could have migrated inward all the way to ~1.5 standing of early Solar System evolution. Historically, AU from the Sun. At that point Jupiter and Saturn it was thought that the planets and small bodies formed could have become trapped in their mutual 2:3 reso- near their current locations. Starting in the 1980’s with nance and would have begun to move outward. pioneering work by Ward, Lin, and Papaloizou, (for The Grand Tack model studied the gravitational planet–gas disk interactions) in the late 1970s and Fer- scattering of asteroids by Jupiter and Saturn during nandez and Ip (for planet–planetesimal disk interac- their inward, then outward migration. This model not tions) in the early 1980s, however, it has now become only reproduces the mass and mixture of spectral types clear that the structure of the Solar System most likely in the asteroid belt, but also truncates the planetesimal changed as the planets grew and migrated [e.g., 1, 2]. disk from which the terrestrial planets form, as in Han- Evidence for giant planet migration can be found in sen’s work. This allowed them to form a low-mass the orbital structures of the Kuiper belt, Trojans, irreg- Mars. -
December 2019 Shop Local
December 2019 Shop Local If you plan to shop for gifts this holiday season, before you go online be sure to check out the unique offerings at local businesses. And don't miss the new Princeton University Art Museum Store location in downtown Princeton. Visit their new store at 56 Nassau Street for artisanal crafts, exhibition- themed merchandise and mission-related gifts - open Sunday-Tuesday from 10:00 am-6:00 pm and Wednesday-Saturday 10:00 am-8:30 pm. Holiday Game Nights Princeton University Athletics offers fans three opportunities to purchase discounted tickets to the following athletic events with donation of a non-perishable food item. All donations support Mercer Street Friends Food Bank. Men's Hockey vs Colorado College Saturday, December 7 at 7 PM Hobey Baker Rink Click to Enlarge Women's Basketball vs. Hartford Tuesday, December 10 at 5 PM Jadwin Gym Men's Basketball vs. Monmouth Tuesday, December 10 at 8 PM Jadwin Gym Lectures George Packer, staff writer at The Atlantic and formerly at The New Yorker, will discuss his new book: Our Man: Richard Holbrooke and the End of the American Century. Monday, December 2; 4:30 pm; Friend Center, Room 101. Professor Anu Ramaswami discusses Sustainable Urban Food Systems and Food Action Planning in the U.S. and India. Tuesday, December 3; 12:30 pm; Guyot Hall, Room 10. The Environmental Humanities Colloquium series continues with Salvage: Experiment, Engagement and the Environmental Humanities. Wednesday, December 4; 4:30 pm; East Pyne, Room 111. The Program in Law and Public Affairs presents Beyond the Bench: Federal Judges, Public Engagement, and Civil Rights. -
Terrestrial Planets in High-Mass Disks Without Gas Giants
A&A 557, A42 (2013) Astronomy DOI: 10.1051/0004-6361/201321304 & c ESO 2013 Astrophysics Terrestrial planets in high-mass disks without gas giants G. C. de Elía, O. M. Guilera, and A. Brunini Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata and Instituto de Astrofísica de La Plata, CCT La Plata-CONICET-UNLP, Paseo del Bosque S/N, 1900 La Plata, Argentina e-mail: [email protected] Received 15 February 2013 / Accepted 24 May 2013 ABSTRACT Context. Observational and theoretical studies suggest that planetary systems consisting only of rocky planets are probably the most common in the Universe. Aims. We study the potential habitability of planets formed in high-mass disks without gas giants around solar-type stars. These systems are interesting because they are likely to harbor super-Earths or Neptune-mass planets on wide orbits, which one should be able to detect with the microlensing technique. Methods. First, a semi-analytical model was used to define the mass of the protoplanetary disks that produce Earth-like planets, super- Earths, or mini-Neptunes, but not gas giants. Using mean values for the parameters that describe a disk and its evolution, we infer that disks with masses lower than 0.15 M are unable to form gas giants. Then, that semi-analytical model was used to describe the evolution of embryos and planetesimals during the gaseous phase for a given disk. Thus, initial conditions were obtained to perform N-body simulations of planetary accretion. We studied disks of 0.1, 0.125, and 0.15 M. -
Women's Basketball
Women’s Basketball Updated: March of 2020 First Game: Feb. 2, 1972 (at Centenary) All-Time Record: 722-546 (.569) Head Coaching Register: W L Pct. Penny Hinckley (1971-74) 15 13 .536 Pat Walsh (1974-79) 72 38 .655 Diane Schumacher (1979-82) 29 52 .358 Jeanne Foley (1982-84) 19 32 .373 Joan Kowalik (1984-1995) 163 121 .574 Elizabeth Feeley (1995-2000) 68 70 .493 Kevin Morris (2000-01) 2 25 .074 Richard Barron (2001-07) 74 91 .448 Courtney Banghart (2007-2019) 254 103 .711 Carla Berube (2019-Current) 26 1 .963 Ivy League Championships (15): 1975, 1976, 1977, 1978, 1985, 1999, 2006, 2010, 2011, 2012, 2013, 2015, 2018, 2019, 2020 NCAA Tournament Appearances (9): 2010, 2011, 2012, 2013, 2015, 2016, 2018, 2019, 2020 Quick Facts: • Basketball was one of the original women’s varsity sports introduced at Princeton in the 1971-72 academic year. The others were crew, field hockey, squash, swimming and tennis. • Princeton won the first four Ivy League championships by winning the annual postseason tournament. The tournament format existed between 1975 and 1982. Double round-robin play determined the champion beginning with the 1982-83 season. •The Tigers’ only league championship of the 1980s was shared with Brown in 1985 when both teams finished with Ivy records of 9-3. • In 1999, Princeton shared the Ivy title with Dartmouth when both teams finished with Ivy records of 11-3. It was the Tigers’ best Ivy record and only League championship of the 1990s. Dartmouth won the playoff game to advance to the NCAA Tournament and did the same in 2006 when the teams shared the regular season title again. -
Symposium on Telescope Science
Proceedings for the 26th Annual Conference of the Society for Astronomical Sciences Symposium on Telescope Science Editors: Brian D. Warner Jerry Foote David A. Kenyon Dale Mais May 22-24, 2007 Northwoods Resort, Big Bear Lake, CA Reprints of Papers Distribution of reprints of papers by any author of a given paper, either before or after the publication of the proceedings is allowed under the following guidelines. 1. The copyright remains with the author(s). 2. Under no circumstances may anyone other than the author(s) of a paper distribute a reprint without the express written permission of all author(s) of the paper. 3. Limited excerpts may be used in a review of the reprint as long as the inclusion of the excerpts is NOT used to make or imply an endorsement by the Society for Astronomical Sciences of any product or service. Notice The preceding “Reprint of Papers” supersedes the one that appeared in the original print version Disclaimer The acceptance of a paper for the SAS proceedings can not be used to imply or infer an endorsement by the Society for Astronomical Sciences of any product, service, or method mentioned in the paper. Published by the Society for Astronomical Sciences, Inc. First printed: May 2007 ISBN: 0-9714693-6-9 Table of Contents Table of Contents PREFACE 7 CONFERENCE SPONSORS 9 Submitted Papers THE OLIN EGGEN PROJECT ARNE HENDEN 13 AMATEUR AND PROFESSIONAL ASTRONOMER COLLABORATION EXOPLANET RESEARCH PROGRAMS AND TECHNIQUES RON BISSINGER 17 EXOPLANET OBSERVING TIPS BRUCE L. GARY 23 STUDY OF CEPHEID VARIABLES AS A JOINT SPECTROSCOPY PROJECT THOMAS C. -
2014-15 Ivy League Women's Basketball CONFERENCE BASKETBALL STATISTICS Through Games of Jan 05, 2015 (All Games)
2014-15 Ivy League Week 9 Women’s Basketball January 5, 2015 STANDINGS THIS WEEK • Princeton (15-0) is one of four undefeated teams in the country, and one of just two with at least 15 Ivy League Overall victories (No. 14 Mississippi State, 17-0). GP Record Win% Home Away GP Record Win% Home Away Neutral Streak Princeton 0 0-0 0.000 0-0 0-0 15 15-0 1.000 4-0 7-0 4-0 W 15 • The Tigers became the first Ivy League women’s Dartmouth 0 0-0 0.000 0-0 0-0 14 9-5 0.643 5-0 3-5 1-0 W 4 basketball team to be ranked in the top-25 in both Cornell 0 0-0 0.000 0-0 0-0 13 8-5 0.615 4-2 4-3 0-0 W 2 polls at the same time, coming in at No. 22 (AP) and Penn 0 0-0 0.000 0-0 0-0 10 6-4 0.600 5-1 1-3 0-0 W 2 No. 24 (Coaches). Harvard 0 0-0 0.000 0-0 0-0 12 6-6 0.500 2-1 1-3 3-2 L 1 Brown 0 0-0 0.000 0-0 0-0 13 5-8 0.385 2-2 2-4 1-1 W 2 • Seven of this week’s eight games will be streamed on The Ivy League Digital Network (ILDN), including Columbia 0 0-0 0.000 0-0 0-0 12 4-8 0.333 4-4 0-4 0-0 L 2 the start of Ivy-play on Saturday, when Princeton Yale 0 0-0 0.000 0-0 0-0 12 4-8 0.333 3-1 1-6 0-1 L 3 hosts Penn and Harvard hosts Dartmouth. -
Formation of Telluric Planets and the Origin of Terrestrial Water
BIO Web of Conferences 2, 01003 (2014) DOI: 10.1051/bioconf/20140201003 C Owned by the authors, published by EDP Sciences, 2014 Formation of telluric planets and the origin of terrestrial water Sean Raymond1;a 1Laboratoire d’Astrophysique de Bordeaux, UMR 5804 Abstract. Simulations of planet formation have failed to reproduce Mars’ small mass (compared with Earth) for 20 years. Here I will present a solution to the Mars problem that invokes large-scale migration of Jupiter and Saturn while they were still embedded in the gaseous protoplanetary disk. Jupiter first migrated inward, then "tacked" and migrated back outward when Saturn caught up to it and became trapped in resonance. If this tack occurred when Jupiter was at 1.5 AU then the inner disk of rocky planetesimals and em- bryos is truncated and the masses and orbits of all four terrestrial planet are quantitatively reproduced. As the giant planets migrate back outward they re-populate the asteroid belt from two different source populations, matching the structure of the current belt. C-type material is also scattered inward to the terrestrial planet-forming zone, delivering about the right amount of water to Earth on 10-50 Myr timescales. 1 Introduction 2 The formation of terrestrial planets As described in the Introduction, the final stages of terrestrial planet formation take place in the presence of any giant planets that may have formed. In addition, it is during this phase that bodies are large enough that during gravitational close encounters they can obtain large eccentricities. Thus, the feeding zones of the terrestrial planets are determined during their final accretion. -
Arxiv:2106.07648V1 [Astro-Ph.EP] 14 Jun 2021 Behaviors from Periodic, E.G., Kepler-1520 B (Rappaport Et Al
Draft version June 16, 2021 Typeset using LATEX default style in AASTeX62 LBT Reveals Large Dust Particles and a High Mass Loss Rate for K2-22 b Everett Schlawin,1 Kate Y. L. Su,1 Terry Herter,2 Andrew Ridden-Harper,2, 3 and Daniel´ Apai1, 4 1Steward Observatory The University of Arizona 933 North Cherry Avenue Tucson, AZ 85721, USA 2Astronomy Department Cornell University Ithaca NY 14853 3Carl Sagan Institute Cornell University Ithaca NY 14853 4Lunar and Planetary Laboratory The University of Arizona 1629 E. University Blvd. Tucson, AZ 85721, USA ABSTRACT The disintegrating planet candidate K2-22 b shows periodic and stochastic transits best explained by an escaping debris cloud. However, the mechanism that creates the debris cloud is unknown. The grain size of the debris as well as its sublimation rate can be helpful in understanding the environment that disintegrates the planet. Here, we present simultaneous photometry with the g band at 0.48 µm and KS band at 2.1 µm using the Large Binocular Telescope. During an event with very low dust activity, we put a new upper limit on the size of the planet of 0.71 R⊕ or 4500 km. We also detected a medium-depth transit which can be used to constrain the dust particle sizes. We find that the median particle size must be larger than about 0.5 to 1.0 µm, depending on the composition of the debris. This leads to a high mass loss rate of about 3 × 108 kg/s that is consistent with hydrodynamic escape models. -
1 Quick Facts Schedule & Results
Ivy League Champions (13): 1975, 1976, 1977, 1978, 1985, 1999, 2006, 2010, 2011, 2012, 2013, 2015, 2018 NCAA Tournament Appearances (7): 2010, 2011, 2012, 2013, 2015, 2016, 2018 CANCUN CHALLENGE - NOV. 22-24 , 2018 - HARD ROCK HOTEL RIVIERA MAYA SCHEDULE & RESULTS Princeton Tigers At A Glance: 2018 Cancun Nov. 6 at Rider ...............................W,89-65 Nov. 11 at GW ..................................L, 64-49 1-3 Princeton: 68.8 PPG, 69.5 Opp. PPG Challenge Nov. 14 SETON HALL ................L, 70-66 #16 DePaul: 75.0 PPG, 82.5 Opp. PPG Nov. 18 at Penn State ......................L, 79-71 (OT) #15 Syracuse: 77.7 PPG, 63.0 Opp PPG Nov. 22 vs. DePaul# .........................11 a.m. Kansas State: 60.7 PPG, 46.0 Opp PPG Nov. 23 vs. Syracuse#.......................1:30 p.m. Nov. 24 vs. Kansas State#................11 a.m. All-Time Series: DePaul leads 2-0 Nov. 28 at Villanova .........................7 p.m. Dec. 2 DAVIDSON ...................2 p.m. Syracuse leads 2-0 Kansas State leads 3-0 Dec. 8 QUINNIPIAC ................7 p.m. Dec. 11 at Monmouth .....................7 p.m. Dec. 15 MARIST .......................5 p.m. A First Look •Princeton last appeared at the Cancun Challenge in 2014, Dec. 19 at St. Francis (NY) ................2 p.m. •Princeton is 1-3 in 2018 after dropping a 79-71 decision winning against Wake Forest, Montana and Charlotte. The Dec. 21 at Hartford ..........................7 p.m. in overtime at Penn State on Sunday. Tigers would go on to finish the regular season at 30-0 and Dec. 29 at New Hampshire..............1 p.m.