Why Pluto Is Not a Planet Anymore Or How Astronomical Objects Get Named
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Chapter 3: Familiarizing Yourself with the Night Sky
Chapter 3: Familiarizing Yourself With the Night Sky Introduction People of ancient cultures viewed the sky as the inaccessible home of the gods. They observed the daily motion of the stars, and grouped them into patterns and images. They assigned stories to the stars, relating to themselves and their gods. They believed that human events and cycles were part of larger cosmic events and cycles. The night sky was part of the cycle. The steady progression of star patterns across the sky was related to the ebb and flow of the seasons, the cyclical migration of herds and hibernation of bears, the correct times to plant or harvest crops. Everywhere on Earth people watched and recorded this orderly and majestic celestial procession with writings and paintings, rock art, and rock and stone monuments or alignments. When the Great Pyramid in Egypt was constructed around 2650 BC, two shafts were built into it at an angle, running from the outside into the interior of the pyramid. The shafts coincide with the North-South passage of two stars important to the Egyptians: Thuban, the star closest to the North Pole at that time, and one of the stars of Orion’s belt. Orion was The Ishango Bone, thought to be a 20,000 year old associated with Osiris, one of the Egyptian gods of the lunar calendar underworld. The Bighorn Medicine Wheel in Wyoming, built by Plains Indians, consists of rocks in the shape of a large circle, with lines radiating from a central hub like the spokes of a bicycle wheel. -
Messier Objects
Messier Objects From the Stocker Astroscience Center at Florida International University Miami Florida The Messier Project Main contributors: • Daniel Puentes • Steven Revesz • Bobby Martinez Charles Messier • Gabriel Salazar • Riya Gandhi • Dr. James Webb – Director, Stocker Astroscience center • All images reduced and combined using MIRA image processing software. (Mirametrics) What are Messier Objects? • Messier objects are a list of astronomical sources compiled by Charles Messier, an 18th and early 19th century astronomer. He created a list of distracting objects to avoid while comet hunting. This list now contains over 110 objects, many of which are the most famous astronomical bodies known. The list contains planetary nebula, star clusters, and other galaxies. - Bobby Martinez The Telescope The telescope used to take these images is an Astronomical Consultants and Equipment (ACE) 24- inch (0.61-meter) Ritchey-Chretien reflecting telescope. It has a focal ratio of F6.2 and is supported on a structure independent of the building that houses it. It is equipped with a Finger Lakes 1kx1k CCD camera cooled to -30o C at the Cassegrain focus. It is equipped with dual filter wheels, the first containing UBVRI scientific filters and the second RGBL color filters. Messier 1 Found 6,500 light years away in the constellation of Taurus, the Crab Nebula (known as M1) is a supernova remnant. The original supernova that formed the crab nebula was observed by Chinese, Japanese and Arab astronomers in 1054 AD as an incredibly bright “Guest star” which was visible for over twenty-two months. The supernova that produced the Crab Nebula is thought to have been an evolved star roughly ten times more massive than the Sun. -
Celestial Navigation (Fall) NAME GROUP
SIERRA COLLEGE OBSERVATIONAL ASTRONOMY LABORATORY EXERCISE Lab N03: Celestial Navigation (Fall) NAME GROUP OBJECTIVE: Learn about the Celestial Coordinate System. Learn about stellar designations. Learn about deep sky object designations. INTRODUCTION: The Horizon Coordinate System is simple, but flawed, because the altitude and azimuth measures of stars change as the sky rotates. Astronomers have developed an improved scheme called the Celestial Coordinate System, which is fixed with the stars. The two coordinates are Right Ascension and Declination. Declination ranges from the North Celestial Pole to the South Celestial Pole, with the Celestial Equator being a line around the sky at the midline of those two extremes. We will use these coordinates when navigating using the SC001 and SC002 charts. There are many ways to designate stars. The most common is called the Bayer designations. The Bayer designation of a star starts with a Greek letter. The brightest star in the constellation gets “alpha” (the first letter in the Greek alphabet), the second brightest star gets “beta,” and so on. (The Greek alphabet is shown below.) The Bayer designation must also include the constellation name. There are only 24 letters in the Greek alphabet, so this system is obviously very limited. The Greek alphabet 1) Alpha 7) Eta 13) Nu 19) Tau 2) Beta 8) Theta 14) Xi 20) Upsilon 3) Gamma 9) Iota 15) Omicron 21) Phi 4) Delta 10) Kappa 16) Pi 22) Chi 5) Epsilon 11) Lambda 17) Rho 23) Psi 6) Zeta 12) Mu 18) Sigma 24) Omega A more extensive naming system is called the Flamsteed designation. -
Apus Constellation Visible at Latitudes Between +5° and -90°
Apus Constellation Visible at latitudes between +5° and -90°. Best visible at 21:00 (9 p.m.) during the month of July. Apus is a small constellation in the southern sky. It represents a bird-of-paradise, and its name means "without feet" in Greek because the bird-of-paradise was once wrongly believed to lack feet. First depicted on a celestial globe by Petrus Plancius in 1598, it was charted on a star atlas by Johann Bayer in his 1603 Uranometria. The French explorer and astronomer Nicolas Louis de Lacaille charted and gave the brighter stars their Bayer designations in 1756. The five brightest stars are all reddish in hue. Shading the others at apparent magnitude 3.8 is Alpha Apodis, an orange giant that has around 48 times the diameter and 928 times the luminosity of the Sun. Marginally fainter is Gamma Apodis, another ageing giant star. Delta Apodis is a double star, the two components of which are 103 arcseconds apart and visible with the naked eye. Two star systems have been found to have planets. Apus was one of twelve constellations published by Petrus Plancius from the observations of Pieter Dirkszoon Keyser and Frederick de Houtman who had sailed on the first Dutch trading expedition, known as the Eerste Schipvaart, to the East Indies. It first appeared on a 35-cm diameter celestial globe published in 1598 in Amsterdam by Plancius with Jodocus Hondius. De Houtman included it in his southern star catalogue in 1603 under the Dutch name De Paradijs Voghel, "The Bird of Paradise", and Plancius called the constellation Paradysvogel Apis Indica; the first word is Dutch for "bird of paradise". -
Lunar & Planetary Surface Power Management & Distribution
NASA SBIR 2020 Phase I Solicitation Z1.05 Lunar & Planetary Surface Power Management & Distribution Lead Center: GRC Participating Center(s): GSFC, JSC Technology Area: TA3 Space Power and Energy Storage Scope Title Innovative ways to transmit high power for lunar & Mars surface missions Scope Description The Global Exploration Roadmap (January 2018) and the Space Policy Directive (December 2017) detail NASA’s plans for future human-rated space missions. A major factor in this involves establishing bases on the lunar surface and eventually Mars. Surface power for bases is envisioned to be located remotely from the habitat modules and must be efficiently transferred over significant distances. The International Space Station (ISS) has the highest power (100kW), and largest space power distribution system with eight interleaved micro-grids providing power functions similar to a terrestrial power utility. Planetary bases will be similar to the ISS with expectations of multiple power sources, storage, science, and habitation modules, but at higher power levels and with longer distribution networks providing interconnection. In order to enable high power (>100kW) and longer distribution systems on the surface of the moon or Mars, NASA is in need of innovative technologies in the areas of lower mass/higher efficiency power electronic regulators, switchgear, cabling, connectors, wireless sensors, power beaming, power scavenging, and power management control. The technologies of interest would need to operate in extreme temperature environments, including lunar night, and could experience temperature changes from -153C to 123C for lunar applications, and -125C to 80C for Mars bases. In addition to temperature extremes, technologies would need to withstand (have minimal degradation from) lunar dust/regolith, Mars dust storms, and space radiation levels. -
The Solar System
5 The Solar System R. Lynne Jones, Steven R. Chesley, Paul A. Abell, Michael E. Brown, Josef Durech,ˇ Yanga R. Fern´andez,Alan W. Harris, Matt J. Holman, Zeljkoˇ Ivezi´c,R. Jedicke, Mikko Kaasalainen, Nathan A. Kaib, Zoran Kneˇzevi´c,Andrea Milani, Alex Parker, Stephen T. Ridgway, David E. Trilling, Bojan Vrˇsnak LSST will provide huge advances in our knowledge of millions of astronomical objects “close to home’”– the small bodies in our Solar System. Previous studies of these small bodies have led to dramatic changes in our understanding of the process of planet formation and evolution, and the relationship between our Solar System and other systems. Beyond providing asteroid targets for space missions or igniting popular interest in observing a new comet or learning about a new distant icy dwarf planet, these small bodies also serve as large populations of “test particles,” recording the dynamical history of the giant planets, revealing the nature of the Solar System impactor population over time, and illustrating the size distributions of planetesimals, which were the building blocks of planets. In this chapter, a brief introduction to the different populations of small bodies in the Solar System (§ 5.1) is followed by a summary of the number of objects of each population that LSST is expected to find (§ 5.2). Some of the Solar System science that LSST will address is presented through the rest of the chapter, starting with the insights into planetary formation and evolution gained through the small body population orbital distributions (§ 5.3). The effects of collisional evolution in the Main Belt and Kuiper Belt are discussed in the next two sections, along with the implications for the determination of the size distribution in the Main Belt (§ 5.4) and possibilities for identifying wide binaries and understanding the environment in the early outer Solar System in § 5.5. -
Theoretical Orbits of Planets in Binary Star Systems 1
Theoretical Orbits of Planets in Binary Star Systems 1 Theoretical Orbits of Planets in Binary Star Systems S.Edgeworth 2001 Table of Contents 1: Introduction 2: Large external orbits 3: Small external orbits 4: Eccentric external orbits 5: Complex external orbits 6: Internal orbits 7: Conclusion Theoretical Orbits of Planets in Binary Star Systems 2 1: Introduction A binary star system consists of two stars which orbit around their joint centre of mass. A large proportion of stars belong to such systems. What sorts of orbits can planets have in a binary star system? To examine this question we use a computer program called a multi-body gravitational simulator. This enables us to create accurate simulations of binary star systems with planets, and to analyse how planets would really behave in this complex environment. Initially we examine the simplest type of binary star system, which satisfies these conditions:- 1. The two stars are of equal mass. 2, The two stars share a common circular orbit. 3. Planets orbit on the same plane as the stars. 4. Planets are of negligible mass. 5. There are no tidal effects. We use the following units:- One time unit = the orbital period of the star system. One distance unit = the distance between the two stars. We can classify possible planetary orbits into two types. A planet may have an internal orbit, which means that it orbits around just one of the two stars. Alternatively, a planet may have an external orbit, which means that its orbit takes it around both stars. Also a planet's orbit may be prograde (in the same direction as the stars' orbits ), or retrograde (in the opposite direction to the stars' orbits). -
Binary and Multiple Systems of Asteroids
Binary and Multiple Systems Andrew Cheng1, Andrew Rivkin2, Patrick Michel3, Carey Lisse4, Kevin Walsh5, Keith Noll6, Darin Ragozzine7, Clark Chapman8, William Merline9, Lance Benner10, Daniel Scheeres11 1JHU/APL [[email protected]] 2JHU/APL [[email protected]] 3University of Nice-Sophia Antipolis/CNRS/Observatoire de la Côte d'Azur [[email protected]] 4JHU/APL [[email protected]] 5University of Nice-Sophia Antipolis/CNRS/Observatoire de la Côte d'Azur [[email protected]] 6STScI [[email protected]] 7Harvard-Smithsonian Center for Astrophysics [[email protected]] 8SwRI [[email protected]] 9SwRI [[email protected]] 10JPL [[email protected]] 11Univ Colorado [[email protected]] Abstract A sizable fraction of small bodies, including roughly 15% of NEOs, is found in binary or multiple systems. Understanding the formation processes of such systems is critical to understanding the collisional and dynamical evolution of small body systems, including even dwarf planets. Binary and multiple systems provide a means of determining critical physical properties (masses, densities, and rotations) with greater ease and higher precision than is available for single objects. Binaries and multiples provide a natural laboratory for dynamical and collisional investigations and may exhibit unique geologic processes such as mass transfer or even accretion disks. Missions to many classes of planetary bodies – asteroids, Trojans, TNOs, dwarf planets – can offer enhanced science return if they target binary or multiple systems. Introduction Asteroid lightcurves were often interpreted through the 1970s and 1980s as showing evidence for satellites, and occultations of stars by asteroids also provided tantalizing if inconclusive hints that asteroid satellites may exist. -
A Bibliometric Perspective Survey of Astronomical Object Tracking System
University of Nebraska - Lincoln DigitalCommons@University of Nebraska - Lincoln Library Philosophy and Practice (e-journal) Libraries at University of Nebraska-Lincoln 2-15-2021 A Bibliometric Perspective Survey of Astronomical Object Tracking System Mariyam Ashai Symbiosis Institute of Technology (SIT), Symbiosis International (Deemed University), Pune, India, [email protected] Rhea Gautam Mukherjee Symbiosis Institute of Technology (SIT), Symbiosis International (Deemed University), Pune, India, [email protected] Sanjana Mundharikar Symbiosis Institute of Technology (SIT), Symbiosis International (Deemed University), Pune, India, [email protected] Vinayak Dev Kuanr Symbiosis Institute of Technology (SIT), Symbiosis International (Deemed University), Pune, India, [email protected] Shivali Amit Wagle Symbiosis Institute of Technology (SIT), Symbiosis International (Deemed University), Pune, India, [email protected] See next page for additional authors Follow this and additional works at: https://digitalcommons.unl.edu/libphilprac Part of the Library and Information Science Commons, and the Other Aerospace Engineering Commons Ashai, Mariyam; Mukherjee, Rhea Gautam; Mundharikar, Sanjana; Kuanr, Vinayak Dev; Wagle, Shivali Amit; and R, Harikrishnan, "A Bibliometric Perspective Survey of Astronomical Object Tracking System" (2021). Library Philosophy and Practice (e-journal). 5151. https://digitalcommons.unl.edu/libphilprac/5151 Authors Mariyam Ashai, Rhea Gautam Mukherjee, Sanjana Mundharikar, -
Guide to the Extended Versions of MPC Data Files Based on the MPCORB Format
Guide to the Extended Versions of MPC Data Files Based on the MPCORB Format Last updated: 2016/04/19 by J.L. Galache Introduction The Minor Planet Center (MPC) has been providing the orbits of minor planets in the form of a file, MPCORB.DAT, since the mid '90s (1990s, not 1890s). Back then there were only a few thousand known asteroids, compared to the several hundred thousand of today, so a flat text file was the appropriate way to circulate these data. It was also a time when most orbit computations were programmed in Fortran, which ingested data no other way. MPCORB.DAT has therefore always been, and continues to be, a fixed-width file (see Table 1 for the current format description1). In fact, all original data files available on the MPC website are flat text files (even the orbits files provided for planetarium-type/sky simulation software packages are simply text files of varying format2). In the early years of the 2010s, possibly due to the rising popularity of the scripting language Python amongst astronomers, and an increased interest from developers wanting to write asteroid-themed tools, requests were received to provide data in other, easier to parse formats, e.g., JSON, CSV, SQL, etc. At the same time, astronomers and developers alike wanted more information than was currently been provided in MPCORB.DAT; information that did exist on the MPC website in other, often hard to find, files. Here was an opportunity to add some new data to existing files, while also making them available in other formats. -
1 Resonant Kuiper Belt Objects
Resonant Kuiper Belt Objects - a Review Renu Malhotra Lunar and Planetary Laboratory, The University of Arizona, Tucson, AZ, USA Email: [email protected] Abstract Our understanding of the history of the solar system has undergone a revolution in recent years, owing to new theoretical insights into the origin of Pluto and the discovery of the Kuiper belt and its rich dynamical structure. The emerging picture of dramatic orbital migration of the planets driven by interaction with the primordial Kuiper belt is thought to have produced the final solar system architecture that we live in today. This paper gives a brief summary of this new view of our solar system's history, and reviews the astronomical evidence in the resonant populations of the Kuiper belt. Introduction Lying at the edge of the visible solar system, observational confirmation of the existence of the Kuiper belt came approximately a quarter-century ago with the discovery of the distant minor planet (15760) Albion (formerly 1992 QB1, Jewitt & Luu 1993). With the clarity of hindsight, we now recognize that Pluto was the first discovered member of the Kuiper belt. The current census of the Kuiper belt includes more than 2000 minor planets at heliocentric distances between ~30 au and ~50 au. Their orbital distribution reveals a rich dynamical structure shaped by the gravitational perturbations of the giant planets, particularly Neptune. Theoretical analysis of these structures has revealed a remarkable dynamic history of the solar system. The story is as follows (see Fernandez & Ip 1984, Malhotra 1993, Malhotra 1995, Fernandez & Ip 1996, and many subsequent works). -
The Minor Planets
The Minor Planets Swinburne Astronomy Online 3D PDF c SAO 2012 The Minor Planets c Swinburne Astronomy Online 2012 1 Description 1.1 Minor planets Our view of the Solar System has changed dramatically over the past 15 years with the discovery of new classes of small bodies. Mi- nor planets are another name for asteroids, or celestial bodies that orbit the Sun that are not otherwise classed as planets or comets. Generally, minor planets are relatively small rocky bodies, while comets are icy bodies that become active when their orbits carry them close to the Sun. (An \active" comet exhibits a large coma and a long tail.) The minor planets can be classified by their orbital characteristics. In this 3D PDF, we have included 5 classes of minor planets: (1) the Near Earth Asteroids (NEAs), (2) the main belt asteroids, (3) the Trojan asteroids of Jupiter, (4) the Centaurs, and (5) the Trans-Neptunian Objects (TNOs). The dataset used comes from the Minor Planets Centre. As of 19 November 2012, there were 9,346 NEAs (comprising 732 Atens, 4686 Apollos and 3928 Amors); 581,613 main belt asteroids; 5,407 jovian Trojans; 330 Centaurs; and 1,150 TNOs. (Note than in this 3D PDF, we have only included 11,678 main belt asteroids.) • The Near Earth Asteroids have perihelion distances of less than 1.3 AU, and include the following sub-classes: { Atens have aphelion distances greater than 0.983 AU, and semi-major axes less than 1 AU { Apollos have perihelion distances less than 1.017 AU, and semi-major axes greater than 1 AU { Amors have perihelion distances between 1.017 and 1.3 AU and semi-major axes greater than 1 AU • The main belt asteroids reside between the orbits of Mars and Jupiter, with most of the asteroids orbiting between about 2.1 AU and 3.3 AU.