Image of Planetary Nebula NGC 7027 with Illustration of Helium Hydride Molecules
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Delite Eyepiece Between 100X and 200X for a Given Tele- Line for Tele Vue Optics
EQUIPMENT REVIEW to help prevent an errant eyepiece from blue, and twin-lobed, somewhat reminis- falling to the ground. cent of the Little Dumbbell Nebula (M76), When I test eyepieces, it’s important to although the emphasis was on the lobes Select these eyepieces to enhance your observing me to use them in a variety of telescopes so rather than the center. without ruining your credit. by Tom Trusock I can understand what aberrations the tele- Finally, I took the time to check the scope adds to the design. Through the contrast with the Fetus Nebula (NGC We test years, I’ve seen amateurs blame specific 7008). With a bright star just off the edge of aberrations on eyepiece design that were this planetary nebula, its large size and low the fault of the telescope. Always remem- surface brightness can make it difficult to ber, we deal with an optical system. pick out the distinctive shape, but it was in Because of this, I’m careful to review eye- clear view through the DeLites. pieces in various telescopes I am already familiar with. For this review, I used an Comparing sizes Tele Vue’s DeLite 18-inch f/4.5 Newtonian reflector These are excellent eyepieces. But which (equipped with the Tele Vue Paracorr), a one did I prefer? I found that my favorite 3.6-inch f/7 apochromatic refractor, and a eyepiece depended greatly on the telescope 6-inch f/15 Maksutov reflector. I used it in. Overall, each DeLite performed My testing showed all three scopes per- similarly, so I matched magnification to formed similarly, so the comments in gen- sky conditions. -
Planetary Nebulae
Planetary Nebulae A planetary nebula is a kind of emission nebula consisting of an expanding, glowing shell of ionized gas ejected from old red giant stars late in their lives. The term "planetary nebula" is a misnomer that originated in the 1780s with astronomer William Herschel because when viewed through his telescope, these objects appeared to him to resemble the rounded shapes of planets. Herschel's name for these objects was popularly adopted and has not been changed. They are a relatively short-lived phenomenon, lasting a few tens of thousands of years, compared to a typical stellar lifetime of several billion years. The mechanism for formation of most planetary nebulae is thought to be the following: at the end of the star's life, during the red giant phase, the outer layers of the star are expelled by strong stellar winds. Eventually, after most of the red giant's atmosphere is dissipated, the exposed hot, luminous core emits ultraviolet radiation to ionize the ejected outer layers of the star. Absorbed ultraviolet light energizes the shell of nebulous gas around the central star, appearing as a bright colored planetary nebula at several discrete visible wavelengths. Planetary nebulae may play a crucial role in the chemical evolution of the Milky Way, returning material to the interstellar medium from stars where elements, the products of nucleosynthesis (such as carbon, nitrogen, oxygen and neon), have been created. Planetary nebulae are also observed in more distant galaxies, yielding useful information about their chemical abundances. In recent years, Hubble Space Telescope images have revealed many planetary nebulae to have extremely complex and varied morphologies. -
A Basic Requirement for Studying the Heavens Is Determining Where In
Abasic requirement for studying the heavens is determining where in the sky things are. To specify sky positions, astronomers have developed several coordinate systems. Each uses a coordinate grid projected on to the celestial sphere, in analogy to the geographic coordinate system used on the surface of the Earth. The coordinate systems differ only in their choice of the fundamental plane, which divides the sky into two equal hemispheres along a great circle (the fundamental plane of the geographic system is the Earth's equator) . Each coordinate system is named for its choice of fundamental plane. The equatorial coordinate system is probably the most widely used celestial coordinate system. It is also the one most closely related to the geographic coordinate system, because they use the same fun damental plane and the same poles. The projection of the Earth's equator onto the celestial sphere is called the celestial equator. Similarly, projecting the geographic poles on to the celest ial sphere defines the north and south celestial poles. However, there is an important difference between the equatorial and geographic coordinate systems: the geographic system is fixed to the Earth; it rotates as the Earth does . The equatorial system is fixed to the stars, so it appears to rotate across the sky with the stars, but of course it's really the Earth rotating under the fixed sky. The latitudinal (latitude-like) angle of the equatorial system is called declination (Dec for short) . It measures the angle of an object above or below the celestial equator. The longitud inal angle is called the right ascension (RA for short). -
Origins of Life in the Universe Zackary Johnson
11/4/2007 Origins of Life in the Universe Zackary Johnson OCN201 Fall 2007 [email protected] Zackary Johnson http://www.soest.hawaii.edu/oceanography/zij/education.html Uniiiversity of Hawaii Department of Oceanography Class Schedule Nov‐2Originsof Life and the Universe Nov‐5 Classification of Life Nov‐7 Primary Production Nov‐9Consumers Nov‐14 Evolution: Processes (Steward) Nov‐16 Evolution: Adaptation() (Steward) Nov‐19 Marine Microbiology Nov‐21 Benthic Communities Nov‐26 Whale Falls (Smith) Nov‐28 The Marine Food Web Nov‐30 Community Ecology Dec‐3 Fisheries Dec‐5Global Ecology Dec‐12 Final Major Concepts TIMETABLE Big Bang! • Life started early, but not at the beginning, of Earth’s Milky Way (and other galaxies formed) history • Abiogenesis is the leading hypothesis to explain the beginning of life on Earth • There are many competing theories as to how this happened • Some of the details have been worked out, but most Formation of Earth have not • Abiogenesis almost certainly occurred in the ocean 20‐15 15‐94.5Today Billions of Years Before Present 1 11/4/2007 Building Blocks TIMETABLE Big Bang! • Universe is mostly hydrogen (H) and helium (He); for Milky Way (and other galaxies formed) example –the sun is 70% H, 28% He and 2% all else! Abundance) e • Most elements of interest to biology (C, N, P, O, etc.) were (Relativ 10 produced via nuclear fusion Formation of Earth Log at very high temperature reactions in large stars after Big Bang 20‐13 13‐94.7Today Atomic Number Billions of Years Before Present ORIGIN OF LIFE ON EARTH Abiogenesis: 3 stages Divine Creation 1. -
S-PROCESS ABUNDANCES in PLANETARY NEBULAE Brian Sharpee,1 Yong Zhang,2, 3, 4 Robert Williams,2 Eric Pellegrini,5 Kenneth Cavagnolo,5 Jack A
The Astrophysical Journal, 659:1265Y1290, 2007 April 20 A # 2007. The American Astronomical Society. All rights reserved. Printed in U.S.A. s-PROCESS ABUNDANCES IN PLANETARY NEBULAE Brian Sharpee,1 Yong Zhang,2, 3, 4 Robert Williams,2 Eric Pellegrini,5 Kenneth Cavagnolo,5 Jack A. Baldwin,5 Mark Phillips,6 and Xiao-Wei Liu 3 Received 2005 May 6; accepted 2006 December 4 ABSTRACT The s-process should occur in all but the lower mass progenitor stars of planetary nebulae, and this should be re- flected in the chemical composition of the gas that is expelled to create the current planetary nebula shell. Weak for- bidden emission lines are expected from several s-process elements in these shells and have been searched for and in some cases detected in previous investigations. Here we extend these studies by combining very high signal-to-noise ratio echelle spectra of a sample of PNe with a critical analysis of the identification of the emission lines of Z > 30 ions. Emission lines of Br, Kr, Xe, Rb, Ba, and Pb are detected with a reasonable degree of certainty in at least some of the objects studied here, and we also tentatively identify lines from Te and I, each in one object. The strengths of these lines indicate enhancement of s-process elements in the central star progenitors, and we determine the abundances of Br, Kr, and Xe, elements for which atomic data relevant for abundance determination have recently become available. As representative elements of the ‘‘light’’ and ‘‘heavy’’s-process peaks, Kr and Xe exhibit similar enhancements over solar values, suggesting that PN progenitors experience substantial neutron exposure. -
New Type of Black Hole Detected in Massive Collision That Sent Gravitational Waves with a 'Bang'
New type of black hole detected in massive collision that sent gravitational waves with a 'bang' By Ashley Strickland, CNN Updated 1200 GMT (2000 HKT) September 2, 2020 <img alt="Galaxy NGC 4485 collided with its larger galactic neighbor NGC 4490 millions of years ago, leading to the creation of new stars seen in the right side of the image." class="media__image" src="//cdn.cnn.com/cnnnext/dam/assets/190516104725-ngc-4485-nasa-super-169.jpg"> Photos: Wonders of the universe Galaxy NGC 4485 collided with its larger galactic neighbor NGC 4490 millions of years ago, leading to the creation of new stars seen in the right side of the image. Hide Caption 98 of 195 <img alt="Astronomers developed a mosaic of the distant universe, called the Hubble Legacy Field, that documents 16 years of observations from the Hubble Space Telescope. The image contains 200,000 galaxies that stretch back through 13.3 billion years of time to just 500 million years after the Big Bang. " class="media__image" src="//cdn.cnn.com/cnnnext/dam/assets/190502151952-0502-wonders-of-the-universe-super-169.jpg"> Photos: Wonders of the universe Astronomers developed a mosaic of the distant universe, called the Hubble Legacy Field, that documents 16 years of observations from the Hubble Space Telescope. The image contains 200,000 galaxies that stretch back through 13.3 billion years of time to just 500 million years after the Big Bang. Hide Caption 99 of 195 <img alt="A ground-based telescope&amp;#39;s view of the Large Magellanic Cloud, a neighboring galaxy of our Milky Way. -
IPHAS Extinction Distances to Planetary Nebulae with Those Obtained by Other Authors Using Different Methods
Astronomy & Astrophysics manuscript no. distance14 c ESO 2018 November 4, 2018 IPHAS extinction distances to Planetary Nebulae C. Giammanco1,12, S. E. Sale2, R. L. M. Corradi1,12, M. J. Barlow3, K. Viironen1,13,14, L. Sabin4, M. Santander-Garc´ıa5,1,12, D. J. Frew6, R. Greimel7, B. Miszalski10, S. Phillipps8, A. A. Zijlstra9, A. Mampaso1,12,J. E. Drew2,10, Q. A. Parker6,11 and R. Napiwotzki10. 1 Instituto de Astrof´ısica de Canarias (IAC), C/ V´ıa L´actea s/n, 38200 La Laguna, Spain e-mail: [email protected] 2 Astrophysics Group, Imperial College London, Blackett Laboratory, Prince Consort Road, London SW7 2AZ, U.K. 3 Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK 4 Instituto de Astronom´ıa, Universidad Nacional Aut´onoma de M´exico, Apdo. Postal 877, 22800 Ensenada, B.C., M´exico 5 Isaac Newton Group of Telescopes, Ap. de Correos 321, 38700 Sta. Cruz de la Palma, Spain 6 Department of Physics, Macquarie University, NSW 2109, Australia 7 Institut f¨ur Physik, Karl-Franzens Universit¨at Graz, Universit¨atsplatz 5, 8010 Graz, Austria 8 Astrophysics Group, Department of Physics, Bristol University, Tyndall Avenue, Bristol, BS8 1TL, U.K. 9 Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, University of Manchester, Oxford Road, M13 9PL, Manchester, U.K. 10 Centre for Astrophysics Research, STRI, University of Hertfordshire, College Lane Campus, Hatfield, AL10 9AB, U.K. 11 Anglo-Australian Observatory, PO Box 296, Epping, NSW 1710, Australia 12 Departamento de Astrof´ısica, Universidad de La Laguna, E-38205 La Laguna, Tenerife, Spain 13 Centro Astron´omico Hispano Alem´an, Calar Alto, C/Jes´us Durb´an Rem´on 2-2, E-04004 Almeria, Spain 14 Centro de Estudios de F´ısica del Cosmos de Arag´on (CEFCA), C/General Pizarro 1-1, E-44001 Teruel, Spain Received September 15, 1996; accepted March 16, 1997 ABSTRACT Aims. -
IPHAS Extinction Distances to Planetary Nebulae
A&A 525, A58 (2011) Astronomy DOI: 10.1051/0004-6361/201014464 & c ESO 2010 Astrophysics IPHAS extinction distances to planetary nebulae C. Giammanco1,12,S.E.Sale2,R.L.M.Corradi1,12,M.J.Barlow3, K. Viironen1,13,14,L.Sabin4, M. Santander-García5,1,12,D.J.Frew6,R.Greimel7, B. Miszalski10, S. Phillipps8, A. A. Zijlstra9, A. Mampaso1,12,J.E.Drew2,10,Q.A.Parker6,11, and R. Napiwotzki10 1 Instituto de Astrofísica de Canarias (IAC), C/ vía Láctea s/n, 38200 La Laguna, Spain e-mail: [email protected] 2 Astrophysics Group, Imperial College London, Blackett Laboratory, Prince Consort Road, London SW7 2AZ, UK 3 Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK 4 Instituto de Astronomía, Universidad Nacional Autónoma de México, Apdo. Postal 877, 22800 Ensenada, B.C., Mexico 5 Isaac Newton Group of Telescopes, Ap. de Correos 321, 38700 Sta. Cruz de la Palma, Spain 6 Department of Physics, Macquarie University, NSW 2109, Australia 7 Institut für Physik, Karl-Franzens Universität Graz, Universitätsplatz 5, 8010 Graz, Austria 8 Astrophysics Group, Department of Physics, Bristol University, Tyndall Avenue, Bristol BS8 1TL, UK 9 Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, University of Manchester, Oxford Road, M13 9PL Manchester, UK 10 Centre for Astrophysics Research, STRI, University of Hertfordshire, College Lane Campus, Hatfield AL10 9AB, UK 11 Anglo-Australian Observatory, PO Box 296, Epping, NSW 1710, Australia 12 Departamento de Astrofísica, Universidad de La Laguna, 38205 La Laguna, Tenerife, Spain 13 Centro Astronómico Hispano Alemán, Calar Alto, C/Jesús Durbán Remón 2-2, 04004 Almeria, Spain 14 Centro de Estudios de Física del Cosmos de Aragón (CEFCA), C/General Pizarro 1-1, 44001 Teruel, Spain Received 19 March 2010 / Accepted 3 July 2010 ABSTRACT Aims. -
X-Ray Observations of the Bipolar Pne NGC 2346 and NGC 7026
Draft version August 10, 2018 A Preprint typeset using LTEX style emulateapj v. 6/22/04 XMM-NEWTON OBSERVATIONS OF THE BIPOLAR PLANETARY NEBULAE NGC2346 AND NGC7026 Robert A. Gruendl1, Mart´ın A. Guerrero2, You-Hua Chu1, and Rosa M. Williams1 Draft version August 10, 2018 ABSTRACT We have obtained X-ray observations of the bipolar planetary nebulae (PNe) NGC 2346 and NGC 7026 with XMM-Newton. These observations detected diffuse X-ray emission from NGC 7026 but not from NGC2346. The X-ray emission from NGC7026 appears to be confined within the bipolar lobes of the PN and has spectral properties suggesting a thermal plasma emitting at a temperature of +0.5 6 1.1−0.2 × 10 K. The X-ray spectrum of NGC 7026 is modeled using nebular and stellar abundances to assess whether a significant amount of nebular material has been mixed into the shocked-wind, but the results of this comparison are not conclusive owing to the small number of counts detected. Observations of bipolar PNe indicate that diffuse X-ray emission is much less likely detected in open- lobed nebulae than closed-lobed nebulae, possibly because open-lobed nebulae do not have strong fast winds or are unable to retain hot gas. Subject headings: planetary nebulae: general — planetary nebulae: individual (NGC 2346, NGC 7026) — X-rays: ISM — stars: winds 1. INTRODUCTION The plasma temperatures implied by their X-ray spectra 6 Planetary nebulae (PNe) consist of the stellar mass are a few times 10 K. In the case of NGC6543, the X-ray lost by their low- or intermediate-mass stellar progen- emission is well resolved, and a clear limb-brightening is itors during late evolutionary stages. -
© American Astronomical Society • Provided by the NASA Astrophysics Data System
THEAsTROPHYSICALJOUR.NAL,408:L105-L107, 1993May10 © 1993. Tho American Astronomical Society. All rights reserved. Printed in U.S.A. 1993ApJ...408L.105G H2 MORPHOLOGY OF YOUNG PLANETARY NEBULAE JAMES R. GRAHAM, 1 ' 2 ' 3 T. M. HERBST,4 •5 K. MATTHEWs,2 G. NEUGEBAUER,2 B. T. SoIFER, 2 E. SERABYN, 6 AND S. BECKWITH4 • 5 Received 1993January5;accepted1993 February24 ABSTRACT The distributions of H2 1-0 S(l) emission in the young planetary nebulae BD +30°3639 and NGC 7027 show ~triking similarities: both have limb-brightened arcs of H2 emission with radii that are about twice those of ~h~ir H; II regions. The extended H 2 emission in both nebulae is attributed to a photodissociation region. Thi.s implies that the neutral envelopes of these young planetaries extend well beyond the edge of the H II region, m contrast to older nebulae where the ionized and molecular gas are more nearly coextensive. The contrast between young an~ old planetarie~ can only be explained if the molecular envelope is inhomoge neous. We endorse a scenano for the evolution of a planetary nebula in which a photodissociation front pro pa~ates ~hrou.gh the clumpy molecular envelope, leaving the ionized core embedded in an envelope of partially iomzed atomic gas and dense molecular knots. In an evolved planetary, the H II region has expanded to en~ulf som~ of the dense molecular knot.s, w~ich can be identified with bright [O 1] and H 2 1-0 S(l) conden sations, while the remnant of the photodissoCiated envelope may be detected as a faint optical halo. -
Rings in the Haloes of Planetary Nebulae
A&A 417, 637–646 (2004) Astronomy DOI: 10.1051/0004-6361:20034420 & c ESO 2004 Astrophysics Rings in the haloes of planetary nebulae R. L. M. Corradi1,P.S´anchez-Bl´azquez2 ,G.Mellema3,,C.Gianmanco4, and H. E. Schwarz5 1 Isaac Newton Group of Telescopes, Ap. de Correos 321, 38700 Sta. Cruz de la Palma, Spain 2 Departamento de Astrof´ısica, Universidad Complutense, 28040, Madrid, Spain e-mail: [email protected] 3 Sterrewacht Leiden, Postbus 9513, 2300 RA Leiden, The Netherlands e-mail: [email protected] 4 Instituto de Astrof´ısica de Canarias, 38200 La Laguna, Tenerife, Spain e-mail: [email protected] 5 Cerro Tololo Inter-American Observatory, NOAO-AURA, Casilla 603, La Serena, Chile e-mail: [email protected] Received 30 September 2003 / Accepted 17 December 2003 Abstract. We present a search for rings or arcs in the haloes of planetary nebulae (PNe). We discovered such structures in eight PNe, tripling the sample of PNe with known rings. This shows that, contrary to what was believed to date, the occurrence of mass loss fluctuations with timescales of 102–103 yrs at the end of the asymptotic giant branch phase (AGB) is common. We estimate a lower limit of the occurrence rate of rings in PN haloes to be ∼35%. Using these new detections and the cases previously known, we discuss the statistical properties of ring systems in PNe haloes. We estimate that the mass modulation producing the rings takes place during the last 10 000 or 20 000 yrs of AGB evolution. -
Quantifying the Origins of Life on a Planetary Scale
Quantifying the origins of life on a planetary scale Caleb Scharfa,1 and Leroy Croninb,1 aColumbia Astrobiology Center, Columbia Astrophysics Laboratory, New York, NY 10027; and bSchool of Chemistry, University of Glasgow, Glasgow, G12 8QQ, United Kingdom Edited by Neta A. Bahcall, Princeton University, Princeton, NJ, and approved May 17, 2016 (received for review November 23, 2015) A simple, heuristic formula with parallels to the Drake Equation is currently impossible to construct a first principles quantitative introduced to help focus discussion on open questions for the origins estimate of an abiogenesis probability for the young Earth. It is of life in a planetary context. This approach indicates a number of also the case that we typically conflate the idea of “microabio- areas where quantitative progress can be made on parameter genesis”— namely, a highly localized assembly of molecular estimation for determining origins of life probabilities, based on structures that meets the minimum criterion for a living system— constraints from Bayesian approaches. We discuss a variety of “micro- with “macro-” or planet-wide abiogenesis. In other words the idea scale” factors and their role in determining “macroscale” abiogenesis of life arising on a planet is treated as a singular event rather than probabilities on suitable planets. We also propose that impact ejecta a possible accumulation of many microscale events, each of which exchange between planets with parallel chemistries and chemical evo- might be considered an origin event in its own right, and are ar- lution could in principle amplify the development of molecular com- guably more accessible through laboratory or modeling investi- plexity and abiogenesis probabilities.