A Planet from Another Galaxy
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Astronomers Find First Planet from Another Galaxy (W/ Video) 18 November 2010
Astronomers find first planet from another galaxy (w/ Video) 18 November 2010 even though the star now finds itself within our own galaxy. It is part of the so-called Helmi stream - a group of stars that originally belonged to a dwarf galaxy that was devoured by our galaxy, the Milky Way, in an act of galactic cannibalism about six to nine billion years ago. The results are published today in Science Express. "This discovery is very exciting," says Rainer Klement of the Max-Planck-Institut für Astronomie (MPIA), who was responsible for the selection of the target stars for this study. "For the first time, astronomers have detected a planetary system in a stellar stream of extragalactic origin. Because of the great distances involved, there are no This artist’s impression shows HIP 13044 b, an confirmed detections of planets in other galaxies. exoplanet orbiting a star that entered our galaxy, the But this cosmic merger has brought an Milky Way, from another galaxy. This planet of extragalactic planet within our reach." extragalactic origin was detected by a European team of astronomers using the MPG/ESO 2.2-metre telescope at The star is known as HIP 13044, and it lies about ESO’s La Silla Observatory in Chile. The Jupiter-like 2000 light-years from Earth in the southern planet is particularly unusual, as it is orbiting a star nearing the end of its life and could be about to be constellation of Fornax (the Furnace). The engulfed by it, giving clues about the fate of our own astronomers detected the planet, called HIP 13044 planetary system in the distant future. -
Mètodes De Detecció I Anàlisi D'exoplanetes
MÈTODES DE DETECCIÓ I ANÀLISI D’EXOPLANETES Rubén Soussé Villa 2n de Batxillerat Tutora: Dolors Romero IES XXV Olimpíada 13/1/2011 Mètodes de detecció i anàlisi d’exoplanetes . Índex - Introducció ............................................................................................. 5 [ Marc Teòric ] 1. L’Univers ............................................................................................... 6 1.1 Les estrelles .................................................................................. 6 1.1.1 Vida de les estrelles .............................................................. 7 1.1.2 Classes espectrals .................................................................9 1.1.3 Magnitud ........................................................................... 9 1.2 Sistemes planetaris: El Sistema Solar .............................................. 10 1.2.1 Formació ......................................................................... 11 1.2.2 Planetes .......................................................................... 13 2. Planetes extrasolars ............................................................................ 19 2.1 Denominació .............................................................................. 19 2.2 Història dels exoplanetes .............................................................. 20 2.3 Mètodes per detectar-los i saber-ne les característiques ..................... 26 2.3.1 Oscil·lació Doppler ........................................................... 27 2.3.2 Trànsits -
Post-Main-Sequence Planetary System Evolution Rsos.Royalsocietypublishing.Org Dimitri Veras
Post-main-sequence planetary system evolution rsos.royalsocietypublishing.org Dimitri Veras Department of Physics, University of Warwick, Coventry CV4 7AL, UK Review The fates of planetary systems provide unassailable insights Cite this article: Veras D. 2016 into their formation and represent rich cross-disciplinary Post-main-sequence planetary system dynamical laboratories. Mounting observations of post-main- evolution. R. Soc. open sci. 3: 150571. sequence planetary systems necessitate a complementary level http://dx.doi.org/10.1098/rsos.150571 of theoretical scrutiny. Here, I review the diverse dynamical processes which affect planets, asteroids, comets and pebbles as their parent stars evolve into giant branch, white dwarf and neutron stars. This reference provides a foundation for the Received: 23 October 2015 interpretation and modelling of currently known systems and Accepted: 20 January 2016 upcoming discoveries. 1. Introduction Subject Category: Decades of unsuccessful attempts to find planets around other Astronomy Sun-like stars preceded the unexpected 1992 discovery of planetary bodies orbiting a pulsar [1,2]. The three planets around Subject Areas: the millisecond pulsar PSR B1257+12 were the first confidently extrasolar planets/astrophysics/solar system reported extrasolar planets to withstand enduring scrutiny due to their well-constrained masses and orbits. However, a retrospective Keywords: historical analysis reveals even more surprises. We now know that dynamics, white dwarfs, giant branch stars, the eponymous celestial body that Adriaan van Maanen observed pulsars, asteroids, formation in the late 1910s [3,4]isanisolatedwhitedwarf(WD)witha metal-enriched atmosphere: direct evidence for the accretion of planetary remnants. These pioneering discoveries of planetary material around Author for correspondence: or in post-main-sequence (post-MS) stars, although exciting, Dimitri Veras represented a poor harbinger for how the field of exoplanetary e-mail: [email protected] science has since matured. -
The Agb Newsletter
THE AGB NEWSLETTER An electronic publication dedicated to Asymptotic Giant Branch stars and related phenomena Official publication of the IAU Working Group on Abundances in Red Giants No. 167 — 1 June 2011 http://www.astro.keele.ac.uk/AGBnews Editors: Jacco van Loon and Albert Zijlstra Editorial Dear Colleagues, It is a pleasure to present you the 167th issue of the AGB Newsletter. As always, it is full of informative and inspiring new results. Looking for a postdoctoral researcher position? There’s one in Tenerife! The next issue is planned to be distributed (hopefully) in early July 2011. Editorially Yours, Jacco van Loon and Albert Zijlstra Food for Thought This month’s thought-provoking statement is: Is there a place for solid hydrogen in circumstellar envelopes? Reactions to this statement or suggestions for next month’s statement can be e-mailed to [email protected] (please state whether you wish to remain anonymous) 1 Refereed Journal Papers The oxygen abundance in the Solar Neighborhood M´onica Rodr´ıguez1 and Gloria Delgado-Inglada1 1INAOE, M´exico We present a homogeneous analysis of the oxygen abundance in five H ii regions and eight planetary nebulae (PNe) located at distances lower than 2 kpc and with available spectra of high quality. We find that both the collisionally excited lines and recombination lines imply that the PNe are overabundant in oxygen by about 0.2 dex. An explanation that reconciles the oxygen abundances derived with collisionally excited lines for H ii regions and PNe with the values found for B-stars, the Sun, and the diffuse ISM requires the presence in H ii regions of an organic refractory dust component that is not present in PNe. -
No Evidence of the Planet Orbiting the Extremely Metal-Poor Extragalactic Star HIP 13044
A&A 562, A129 (2014) Astronomy DOI: 10.1051/0004-6361/201322132 & c ESO 2014 Astrophysics No evidence of the planet orbiting the extremely metal-poor extragalactic star HIP 13044 M. I. Jones1,2 and J. S. Jenkins2 1 Departamento de Astronomía y Astrofísica, Pontificia Universidad Católica de Chile, Av. Vicuña Mackenna 4860, 782-0436 Macul, Santiago, Chile e-mail: [email protected] 2 Departamento de Astronomía, Universidad de Chile, Camino El Observatorio 1515, Las Condes, Casilla 36-D Santiago, Chile Received 25 June 2013 / Accepted 25 August 2013 ABSTRACT Context. The recent discovery of three giant planets orbiting the extremely metal-poor stars HIP 11952 and HIP 13044 have chal- lenged theoretical predictions of the core-accretion model. According to this, the metal content of the protoplanetary disk from which giant planets are formed is a key ingredient for the early formation of planetesimals prior to the runaway accretion of the surrounding gas. Aims. We reanalyzed the original FEROS data that were used to detect the planets to prove or refute their existence, employing our new reduction and analysis methods. Methods. We applied the cross-correlation technique to FEROS spectra to measure the radial velocity variation of HIP 13044 and HIP 11952. We reached a typical precision of ∼35 m s−1 for HIP 13044 and ∼25 m s−1 for HIP 11952, which is significantly superior to the uncertainties presented previously. Results. We found no evidence of the planet orbiting the metal-poor extragalactic star HIP 13044. We show that given our radial ve- locity precision, and considering the large number of radial velocity epochs, the probability for a non-detection of the radial velocity signal recently claimed is lower than 10−4. -
Planetary Report : Peter Tagger Scientists Not Only in Interpreting More Than 30 Years and Harry Ashmore
The PLANETARY REPOR T Volume XXXI Number 1 January/February 2011 Mapping Pluto From The Editor arl Sagan, Bruce Murray, and Lou On the Cover CFriedman may have founded the Planetary Society, but it did not spring Pluto is not just a puny ball of ice and rock with a crazy fullly grown from their heads. They orbit on the fringes of our solar system; it is a dynamic had the help of some extraordinary world undergoing dramatic surface and atmospheric people who knew how to build “con - changes. These recent Hubble Space Telescope (HST) stituency groups,” and through their maps of Pluto, shown in a rotational order spaced 40 wisdom, this organization was born. degrees of longitude apart, reveal marked differences Two people in particular shaped what from observations made in the early 1990s, when HST became the prime benefit of member - was new on the job. These invaluable maps will help ship, The Planetary Report : Peter Tagger scientists not only in interpreting more than 30 years and Harry Ashmore. of Pluto observations from other telescopes but also Peter set up the membership side in picking out the best features on which to train New of operations and was the greatest Horizons ’ cameras when it flies by the dwarf planet (and most patient) teacher I have ever in 2015. Images: M. Buie/NASA/STScI/HST known. Harry was a Pulitzer Prize – winning journalist and an avuncular Background guide to non-profit publishing. They The lunar eclipse of December 21, 2010 (Eastern Stan - helped in many ways, but one contri - dard Time) coincided, for the first time since 1638, with bution was their most lasting: they the northern winter solstice. -
Photometry Using Mid-Sized Nanosatellites
Feasibility-Study for Space-Based Transit Photometry using Mid-sized Nanosatellites by Rachel Bowens-Rubin Submitted to the Department of Earth, Atmospheric, and Planetary Science in partial fulfillment of the requirements for the degree of Masters of Science in Earth, Atmospheric, and Planetary Science at the MASSACHUSETTS INSTITUTE OF TECHNOLOGY June 2012 @ Massachusetts Institute of Technology 2012. All rights reserved. A uthor .. ............... ................ Department of Earth, Atmospheric, and Planetary Science May 18, 2012 C ertified by .................. ........ ........................... Sara Seager Professor, Departments of Physics and EAPS Thesis Supervisor VIZ ~ Accepted by.......,.... Robert D. van der Hilst Schulumberger Professor of Geosciences and Head, Department of Earth, Atmospheric, and Planetary Science 2 Feasibility-Study for Space-Based Transit Photometry using Mid-sized Nanosatellites by Rachel Bowens-Rubin Submitted to the Department of Earth, Atmospheric, and Planetary Science on May 18, 2012, in partial fulfillment of the requirements for the degree of Masters of Science in Earth, Atmospheric, and Planetary Science Abstract The photometric precision needed to measure a transit of small planets cannot be achieved by taking observations from the ground, so observations must be made from space. Mid-sized nanosatellites can provide a low-cost option for building an optical system to take these observations. The potential of using nanosatellites of varying sizes to perform transit measurements was evaluated using a theoretical noise budget, simulated exoplanet-transit data, and case studies to determine the expected results of a radial velocity followup mission and transit survey mission. Optical systems on larger mid-sized nanosatellites (such as ESPA satellites) have greater potential than smaller mid-sized nanosatellites (such as CubeSats) to detect smaller planets, detect planets around dimmer stars, and discover more transits in RV followup missions. -
December 2017 BRAS Newsletter
Novemb December 2017 Issue Christmas Party Pot-Luck Monday, December 11th at 7PM at HRPO er 2017 Issue nd (Monthly meetings are on 2 Mondays, Highland Road Park Observatory) . Club provides the meat and drinks. Everyone who wishes to share, please bring a dish. Go ahead and wear your electric tie, Santa hat, elf shoes, whatever. Just come. Family members welcome. What's In This Issue? President’s Message Secretary's Summary Outreach Report Light Pollution Committee Report Recent Forum Entries 20/20 Vision Campaign Messages from the HRPO Friday Night Lecture Series Globe at Night HRPO 20th Anniversary Adult Astronomy Courses Observing Notes – Fornax – The Furnace & Mythology Like this newsletter? See past issues back to 2009 at http://brastro.org/newsletters.html Newsletter of the Baton Rouge Astronomical Society December 2017 President’s Message Well, here it is, the end of my 2-year term as President of BRAS.I feel that I have done a good job, and have helped improve and expand BRAS. HRPO celebrates its 20th Anniversary on Friday, December 29th. Hope to see all of you there to support the Observatory and all it does for BRAS and the public. Modifications to the telescope from AL are going slow due to hard to find material required. BRAS will keep you informed as to its progress. BRAS is back in full swing for our Sidewalk Astronomy outreach. On November 28th we held the third outreach for the season. Watch for announcements of future outreaches in the Night Visions, and come out to support BRAS. Our first interstellar visitor, now leaving our system, has been named 1I/’Oumuamua. -
A Planetary System from the Early Universe
A planetary system from the early Universe A group of European astronomers has discovered an ancient planetary system that is likely to be a survivor from one of the earliest cosmic eras, 13 billion years ago. The system consists of the star HIP 11952 and two planets, which have orbital periods of 290 and 7 days, respectively. Whereas planets usually form within clouds that include heavier chemical elements, the star HIP 11952 contains very little other than hydrogen and helium. The system promises to shed light on planet formation in the early universe – under conditions quite different from those of later planetary systems, such as our own. It is widely accepted that planets are formed in disks of gas and dust that swirl around young stars. But look into the details, and many open questions remain – including the question of what it actually takes to make a planet. With a sample of, by now, more than 750 confirmed planets orbiting stars other than the Sun, astronomers have some idea of the diversity among planetary systems. But also, certain trends have emerged: Statistically, a star that contains more “metals” - in astronomical parlance, the term includes all chemical elements other than hydrogen and helium – is more likely to have planets. This suggests a key question: Originally, the universe contained almost no chemical elements other than hydrogen and helium. Almost all heavier elements have been produced, over time inside stars, and then flung into space as massive stars end their lives in giant explosions (supernovae). So what -
How Far Away Is It (Index)
Index Item Page Link 2dF Galaxy Redshift Survey 15-29 Classroom Aid - Fabric of the Cosmos Accelerating Space Expansion 15-19 Classroom Aid - Accelerating Expansion Accretion Disk 9-13 Classroom Aid - Black Holes Age of the Universe 12-22 Classroom Aid - Hubble's Law Andromeda - Milky Way Collision 14-21 Classroom Aid - Andromeda Milky Way Collision Andromeda Galaxy 10-2 Classroom Aid - The Andromeda Galaxy Anemic Spiral 13-12 Classroom Aid - NGC 4921 Antennae Galaxies 14-6 Classroom Aid - Antennae Galaxies Arches Cluster 7-23 Classroom Aid - Open Star Clusters Asteroid Belt 2-15 Classroom Aid - Asteroid Belt Asteroid Moons 2-16 Classroom Aid - Asteroid Belt Asteroid, 2010 TK7 2-16 Classroom Aid - Lagrange Points Asteroid, Trojan 2-17 Classroom Aid - Lagrange Points Astronomical Unit 2-8 Classroom Aid - Planets and Moons Astrophotography 6-1 Classroom Aid - Astrophotography Atmospheric Distances 1-6 Classroom Aid - How high is the sky Aurora Australis 3-6 Classroom Aid - Aurora Borealis Aurora Borealis 3-6 Classroom Aid - Aurora Borealis Bar Core 9-17 Classroom Aid - Milky Way Disc Structure Barycenter 4-6 Classroom Aid - Stellar Mass Bennu 2-14 Classroom Aid - Asteroid Belt Bessel, Fredrich 4-2 Classroom Aid - Stellar Parallax Binary Star 4-5 Classroom Aid - Stellar Mass Binary Star Mass 4-6 Classroom Aid - Stellar Mass Black Hole MAXI J1820+070 9-15 Classroom Aid - Stellar Mass Black Hole J1820 Black Holes 9-10 Classroom Aid - Black Holes Blackbody Radiation 5-6 Classroom Aid - Star Color and Blackbody Radiation Blue Horsehead Nebula IC 4592 8-5 Classroom Aid - Rho Ophiuchi Blue Stragglers. -
Detection-And-Characterization-Of
UNIVERSIDAD DE CHILE FACULTAD DE CIENCIAS FÍSICAS Y MATEMÁTICAS DEPARTAMENTO DE ASTRONOMÍA DETECTION AND CHARACTERIZATION OF SINGLE AND DOUBLE STELLAR/PLANETARY SYSTEMS TESIS PARA OPTAR AL GRADO DE DOCTORA EN CIENCIAS, MENCIÓN ASTRONOMÍA MARITZA GABRIELA SOTO VÁSQUEZ PROFESOR GUÍA: JAMES STEWART JENKINS MIEMBROS DE LA COMISIÓN: GUILLEM ANGLADA-ESCUDÉ RICARDO RODRIGO MUÑOZ VIDAL PATRICIO MICHEL ROJO RUBKE Este trabajo ha sido parcialmente financiado por CONICYT-PCHA/Doctorado Nacional/2014-21141037 SANTIAGO DE CHILE 2018 RESUMEN DE LA MEMORIA PARA OPTAR AL TÍTULO DE DOCTORA EN CIENCIAS, MENCIÓN ASTRONOMÍA POR: MARITZA GABRIELA SOTO VÁSQUEZ FECHA: 20 DE JUNIO, 2018 PROF. GUÍA: JAMES STEWART JENKINS DETECTION AND CHARACTERIZATION OF SINGLE AND DOUBLE STELLAR/PLANETARY SYSTEMS El crecimiento exponencial del número de exoplanetas descubiertos en los últimos años ha derivado en un mayor entendimiento de los planetas en la galaxia, de los cuales la Tierra es miembro; pero aún nos queda un gran camino por delante. El propósito de esta tesis es descubrir y confirmar nuevos planetas orbitando estrellas enanas y gigantes, además de desarrollar técnicas para extraer la mayor cantidad de información posible de las estrellas, permitiendo así una mayor compresión de los sistemas planetarios en estudio. Primero, analizamos datos crudos tomados con FEROS de las estrellas HD 11977, HD 47536, HD 110014, y HD122430, todas con al menos un planeta descubierto. Confirmamos la existencia de los planetas orbitando a HD 11977, HD 47536 y HD 110012, pero con parámetros orbitales distintos a los publicados. Además, no encontramos evidencia que respaldara la existencia del segundo planeta orbitando a HD 47536, ni que hubiese planetas alrededor de HD 122430 y HD 70573. -
A Giant Planet Around a Metal-Poor Star of Extragalactic Origin
A Giant Planet Around a Metal-poor Star of Extragalactic Origin Johny Setiawan,1∗, Rainer J. Klement1, Thomas Henning1, Hans-Walter Rix1, Boyke Rochau1, Jens Rodmann2, Tim Schulze-Hartung1 1Max-Planck-Institut fur¨ Astronomie Konigstuhl¨ 17, 69117 Heidelberg, Germany 2European Space Agency, Space Environment and Effects Section, ESTEC Keplerlaan 1, 2201 AZ Noordwijk, The Netherlands ∗To whom correspondence should be addressed; E-mail: [email protected]. Stars in their late stage of evolution, such as Horizontal Branch stars, are still largely unexplored for planets. We report the detection of a planetary compan- ion around HIP 13044, a very metal-poor star on the red Horizontal Branch, based on radial velocity observations with a high-resolution spectrograph at the 2.2-m MPG/ESO telescope. The star's periodic radial velocity variation of P = 16.2 days caused by the planet can be distinguished from the peri- ods of the stellar activity indicators. The minimum mass of the planet is 1.25 Mjup and its orbital semi-major axis 0.116 AU. Because HIP 13044 belongs to a group of stars that have been accreted from a disrupted satellite galaxy of the Milky Way, the planet most likely has an extragalactic origin. In the last two decades, several hundred planets have been detected beyond our Solar- system. Most of these extra-solar planets orbit sun-like stars. A small number have been de- 1 tected around stars that are in their late evolutionary state, such as Red Giant Branch (RGB) stars and pulsars. The phase directly after the RGB stage, the Horizontal Branch (HB), how- ever, is still unexplored; therefore, there is no empirical evidence for whether close-in planets, i.e., those with semi-major axes less than 0.1 AU, survive the giant phase of their host stars.