DOCSLIB.ORG

Testing Proposed Planetary Systems – to Destruction

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Testing Proposed Planetary Systems – to Destruction View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by University of Southern Queensland ePrints HORNER ET AL.: EXOPLANS ET HORNER ET AL.: EXOPLANS ET Testing proposed planetary systems – to destruction J Horner, R A Wittenmyer, J P Marshall, T C Hinse and P Robertson examine the dynamics of exoplanet systems and find that some of them don’t last long. The stability of planetary systems offers a check on the likelihood of proposed multiple-exoplanet systems. he detection of planets around other ical derivation of Kepler’s Laws of Planetary future (and past) behaviour. stars is, to many, the single most exciting Motion, which Kepler had proposed almost a In a coarse sense, two broad types of behav­ Tastronomical discovery of our times. For century earlier. The science of orbital mechan­ iour are observed for objects moving in systems millennia, people have asked whether we are ics studies the gravitational interaction between of three or more bodies. Stable orbits show very Downloaded from alone in the universe, and while we do not yet planets, stars and smaller bodies in planetary little modification on long timescales, such know the answer to that question, the detection systems (comets and asteroids). Once a system that the objects moving on those orbits would of these exoplanets surely brings that answer contains more than two bodies, it is no longer be expected to be moving on the same (or very within our grasp. Indeed, we are the first genera­ possible to exactly solve for the motion of all similar) orbits were the observer to return in tion to be able to gaze up at the night sky and those bodies as they interact under the influ­ a billion years, or ten billion years. Unstable know that planets orbit most of the stars we see. ence of gravity. This conundrum is known as the orbits, by contrast, exhibit dramatic variations http://astrogeo.oxfordjournals.org/ Since 1992, when the first planets or planet­ three ­body problem, and essentially means that as time goes by. esimals were found orbiting a pulsar, around it is impossible to predict, on long timescales, In reality, on long enough timescales, almost fifteen hundred exoplanets have been discov­ the motion of the planets around the Sun, or the all orbits become unstable; stability is actually a ered, using two principal techniques: periodic dynamical evolution of exoplanetary systems. sliding scale, from the very unstable to the very radial velocity variations in the motion of A simple example of the problems inherent stable. An example of a very stable orbit would their host stars determined by the mass of the in studies of orbital mechanics is to consider be that of the Earth around the Sun. Although unseen orbiting planet; and the slight drop in a simplified version of our solar system: the the orbit of the Earth is constantly nudged and light from the host star when a planet crosses Sun, the planet Jupiter, and a small object such tweaked by the gravitational influence of all its face. As time has passed, a handful of other as a comet. Consider two versions of the sys­ of the other objects in the solar system, it has by Jenni Thistlewood on January 5, 2015 techniques have begun to be used in the search tem, absolutely identical except for the initial remained essentially unchanged since the for­ for exoplanets. Aside from direct imaging, all location of the small object. In one system, the mation of the solar system, and it is highly likely of the techniques are indirect, detecting the small object is displaced from its location in the to remain so until the Sun becomes a red giant influence of the unseen planet on its host star other by a single atomic radius, with all other star. At the other extreme, the solar system’s or on light from background stars. At the same quantities (the velocities, masses and locations cometary bodies provide numerous examples time, an increasing number of multiple­planet of the objects considered) remaining identical. of highly unstable orbits, continually being systems have been discovered – a scenario that At that instant, the two particles in the two thrown on to new orbits as a result of chaotic provides for a new test to be applied to exam­ planetary systems will experience forces acting inter actions with the planets. Indeed, most com­ ine the veracity of the claimed planets. When on them that differ very slightly, as a result of ets are eventually ejected from the solar system more than one planet is identified in a given their minutely different distances from the Sun entirely as a result of a close encounter with the exoplanetary system, it is possible to examine and from Jupiter. As a result, they will expe­ giant planet Jupiter – our system’s biggest, bad­ the mutual gravitational interaction between rience slightly different accelerations, causing dest bully. the planets. If they are real, and the proposed their orbits to gradually drift apart. The further Typically in these systems, objects whose orbits a fair reflection of the true architecture apart the objects move, the more disparate the orbits are widely separated exhibit significantly of the system, it is reasonable to assume that forces they experience, and the more dramati­ greater dynamical stability than those whose the planetary orbits must be dynamically sta­ cally their orbits will diverge. orbits are closely packed. Furthermore, objects ble on timescales comparable to the age of the Because the initial location, mass and velocity moving on orbits with low eccentricity (i.e. planetary system. By contrast, if the proposed of every single object in a given planetary system circular, or near­circular orbits) are typically planets in a given system become unstable on cannot be precisely known, it is impossible to more dynamically stable than those moving on timescales far shorter than the age of the system, determine how those objects will evolve under eccentric orbits. The most extreme instability then it would be reasonable to conclude that the influence of their mutual gravitational pulls typically occurs when the orbits of two objects those planets are unlikely to exist – at least on on long timescales. But all is not lost. The gravi­ cross one another, or approach one another the proposed orbits. tational evolution of planetary systems (or test particularly closely. In those cases, there is the particles therein) can be modelled computation­ possibility that these objects will eventually Orbital dynamics and stability ally, allowing a wide range of initial conditions experience a close encounter, leading to signifi­ When Sir Isaac Newton published Philosophiæ to be tested. The more tightly packed the initial cant changes in their orbits. Naturalis Principia Mathematica in 1687, he conditions, the longer the different solutions The situation is complicated by orbital res­ laid out the mathematical tools that allow us to will take to diverge and so the better we can tie onances, such as the interaction between the understand fully the motion of objects orbiting down the initial motion of the objects in ques­ giant planet Neptune and the dwarf planet stars. In particular, they allowed the mathemat­ tion, and the better we can understand their Pluto. The orbit of Pluto crosses that of 4.30 A&G • August 2014 • Vol. 55 HORNER ET AL.: EXOPLANS ET Downloaded from http://astrogeo.oxfordjournals.org/ by Jenni Thistlewood on January 5, 2015 Neptune, such that the dwarf planet spends 1: Artist’s impression of the PLATO mission to covery process of the Anglo­Australian Planet approximately 20 years of each ~248­year orbit explore exoplanets. Announced in February Search programme, and have also tested a num­ interior to the orbit of Neptune, and the rest of by the European Space Agency and due to ber of the multiple­planet systems proposed over launch in 2024, PLATO will observe around the time exterior. Normally, one would expect a million stars to find and characterize new the past few years to see whether they stand such a situation to be untenable in the long term planets. (Mark A Garlick) up to dynamical scrutiny. For some systems, – eventually, the two objects would be expected dynamical simulations simply reveal that the to experience a close encounter and disruption proposed planets are dynamically stable across of their orbits, or even a collision. However, years old. As such, given that the planets orbit­ the whole range of orbital architectures allowed Pluto is actually protected from experiencing ing them can reasonably be expected to have by the observational data. More interestingly, close encounters with Neptune because they formed at around the same time as their host in several cases, we have found that dynami­ are trapped in mutual 3:2 mean motion reso­ star, it is reasonable to expect that their orbits cal studies can enable us to more effectively nance. In the time it takes Neptune to complete would be stable on timescales comparable to constrain the orbits of the proposed planets. three orbits of the Sun, Pluto completes two – a the age of their host system. Conversely, the Finally, in several cases, we have found that the commensurability between their orbital peri­ likelihood of discovering planets as they move proposed planetary systems are not dynamically ods that ensures that, whenever Pluto is cross­ towards destruction on dynamically unstable feasible, indicating either that the proposed ing the orbit of Neptune, that giant planet is orbits during the last few thousand years of their planets do not exist, or that they are moving on far away. Despite the fact their orbits cross, the life is very low.
Load more

Recommended publications
  • Naming the Extrasolar Planets
    Naming the extrasolar planets W. Lyra Max Planck Institute for Astronomy, K¨onigstuhl 17, 69177, Heidelberg, Germany [email protected] Abstract and OGLE-TR-182 b, which does not help educators convey the message that these planets are quite similar to Jupiter. Extrasolar planets are not named and are referred to only In stark contrast, the sentence“planet Apollo is a gas giant by their assigned scientific designation. The reason given like Jupiter” is heavily - yet invisibly - coated with Coper- by the IAU to not name the planets is that it is consid- nicanism. ered impractical as planets are expected to be common. I One reason given by the IAU for not considering naming advance some reasons as to why this logic is flawed, and sug- the extrasolar planets is that it is a task deemed impractical. gest names for the 403 extrasolar planet candidates known One source is quoted as having said “if planets are found to as of Oct 2009. The names follow a scheme of association occur very frequently in the Universe, a system of individual with the constellation that the host star pertains to, and names for planets might well rapidly be found equally im- therefore are mostly drawn from Roman-Greek mythology. practicable as it is for stars, as planet discoveries progress.” Other mythologies may also be used given that a suitable 1. This leads to a second argument. It is indeed impractical association is established. to name all stars. But some stars are named nonetheless. In fact, all other classes of astronomical bodies are named.
    [Show full text]
  • Download This Article in PDF Format
    A&A 562, A92 (2014) Astronomy DOI: 10.1051/0004-6361/201321493 & c ESO 2014 Astrophysics Li depletion in solar analogues with exoplanets Extending the sample, E. Delgado Mena1,G.Israelian2,3, J. I. González Hernández2,3,S.G.Sousa1,2,4, A. Mortier1,4,N.C.Santos1,4, V. Zh. Adibekyan1, J. Fernandes5, R. Rebolo2,3,6,S.Udry7, and M. Mayor7 1 Centro de Astrofísica, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal e-mail: [email protected] 2 Instituto de Astrofísica de Canarias, C/ Via Lactea s/n, 38200 La Laguna, Tenerife, Spain 3 Departamento de Astrofísica, Universidad de La Laguna, 38205 La Laguna, Tenerife, Spain 4 Departamento de Física e Astronomia, Faculdade de Ciências, Universidade do Porto, 4169-007 Porto, Portugal 5 CGUC, Department of Mathematics and Astronomical Observatory, University of Coimbra, 3049 Coimbra, Portugal 6 Consejo Superior de Investigaciones Científicas, CSIC, Spain 7 Observatoire de Genève, Université de Genève, 51 ch. des Maillettes, 1290 Sauverny, Switzerland Received 18 March 2013 / Accepted 25 November 2013 ABSTRACT Aims. We want to study the effects of the formation of planets and planetary systems on the atmospheric Li abundance of planet host stars. Methods. In this work we present new determinations of lithium abundances for 326 main sequence stars with and without planets in the Teff range 5600–5900 K. The 277 stars come from the HARPS sample, the remaining targets were observed with a variety of high-resolution spectrographs. Results. We confirm significant differences in the Li distribution of solar twins (Teff = T ± 80 K, log g = log g ± 0.2and[Fe/H] = [Fe/H] ±0.2): the full sample of planet host stars (22) shows Li average values lower than “single” stars with no detected planets (60).
    [Show full text]
  • 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
    [Show full text]
  • AMD-Stability and the Classification of Planetary Systems
    A&A 605, A72 (2017) DOI: 10.1051/0004-6361/201630022 Astronomy c ESO 2017 Astrophysics& AMD-stability and the classification of planetary systems? J. Laskar and A. C. Petit ASD/IMCCE, CNRS-UMR 8028, Observatoire de Paris, PSL, UPMC, 77 Avenue Denfert-Rochereau, 75014 Paris, France e-mail: [email protected] Received 7 November 2016 / Accepted 23 January 2017 ABSTRACT We present here in full detail the evolution of the angular momentum deficit (AMD) during collisions as it was described in Laskar (2000, Phys. Rev. Lett., 84, 3240). Since then, the AMD has been revealed to be a key parameter for the understanding of the outcome of planetary formation models. We define here the AMD-stability criterion that can be easily verified on a newly discovered planetary system. We show how AMD-stability can be used to establish a classification of the multiplanet systems in order to exhibit the planetary systems that are long-term stable because they are AMD-stable, and those that are AMD-unstable which then require some additional dynamical studies to conclude on their stability. The AMD-stability classification is applied to the 131 multiplanet systems from The Extrasolar Planet Encyclopaedia database for which the orbital elements are sufficiently well known. Key words. chaos – celestial mechanics – planets and satellites: dynamical evolution and stability – planets and satellites: formation – planets and satellites: general 1. Introduction motion resonances (MMR, Wisdom 1980; Deck et al. 2013; Ramos et al. 2015) could justify the Hill-type criteria, but the The increasing number of planetary systems has made it nec- results on the overlap of the MMR island are valid only for close essary to search for a possible classification of these planetary orbits and for short-term stability.
    [Show full text]
  • September 2016 BRAS Newsletter
    September 2016 Issue th Next Meeting: Monday, Sept. 12 at 7PM at HRPO (2nd Mondays, Highland Road Park Observatory) What's In This Issue? Due to the 1000 Year Flood in Louisiana beginning August 14, some of our club’s activities were curtailed, thus our newsletter is shorter than usual. President’s Message Secretary's Summary for August (no meeting) Light Pollution Committee Report Outreach Report Photo Gallery 20/20 Vision Campaign Messages from the HRPO Triple Conjunction with Moon Observing Notes: Capricornus – The Sea Goat, by John Nagle & Mythology Newsletter of the Baton Rouge Astronomical Society September 2016 BRAS President’s Message This has been a month of many changes for all of us. Some have lost almost everything in the flood, Some have lost a little, and some have lost nothing... Our hearts go out to all who have lost, and thanks to all who have reached out to help others. Due to the flooding, last month’s meeting, at LIGO, was cancelled. The September meeting will be on the 12th at the Observatory, which did not receive any water during the flood, thus BRAS suffered no loss of property. As part of our Outreach effort. If anyone you know has any telescope and/or equipment that was in water during the flood, let us know and we will try to help clean, adjust, etc. the equipment. On September 2nd (I am a little late with this message), Dr. Alan Stern, the New Horizons Primary Investigator, gave two talks at LSU. The morning talk was for Astronomy graduate students, and was a little technical.
    [Show full text]
  • Density Estimation for Projected Exoplanet Quantities
    Density Estimation for Projected Exoplanet Quantities Robert A. Brown Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 [email protected] ABSTRACT Exoplanet searches using radial velocity (RV) and microlensing (ML) produce samples of “projected” mass and orbital radius, respectively. We present a new method for estimating the probability density distribution (density) of the un- projected quantity from such samples. For a sample of n data values, the method involves solving n simultaneous linear equations to determine the weights of delta functions for the raw, unsmoothed density of the unprojected quantity that cause the associated cumulative distribution function (CDF) of the projected quantity to exactly reproduce the empirical CDF of the sample at the locations of the n data values. We smooth the raw density using nonparametric kernel density estimation with a normal kernel of bandwidth σ. We calibrate the dependence of σ on n by Monte Carlo experiments performed on samples drawn from a the- oretical density, in which the integrated square error is minimized. We scale this calibration to the ranges of real RV samples using the Normal Reference Rule. The resolution and amplitude accuracy of the estimated density improve with n. For typical RV and ML samples, we expect the fractional noise at the PDF peak to be approximately 80 n− log 2. For illustrations, we apply the new method to 67 RV values given a similar treatment by Jorissen et al. in 2001, and to the 308 RV values listed at exoplanets.org on 20 October 2010. In addition to an- alyzing observational results, our methods can be used to develop measurement arXiv:1011.3991v3 [astro-ph.IM] 21 Mar 2011 requirements—particularly on the minimum sample size n—for future programs, such as the microlensing survey of Earth-like exoplanets recommended by the Astro 2010 committee.
    [Show full text]
  • Archival VLT/Naco Multiplicity Investigation of Exoplanet Host Stars J
    Astronomy & Astrophysics manuscript no. final_version c ESO 2018 November 27, 2018 Archival VLT/NaCo multiplicity investigation of exoplanet host stars J. Dietrich1; 2 and C. Ginski1; 3 1 Leiden Observatory, Leiden University, P.O. Box 9513, 2300 RA Leiden, The Netherlands e-mail: [email protected] 2 Harvard University, Cambridge, MA 02138, United States 3 Anton Pannekoek Institute for Astronomy, University of Amsterdam, Science Park 904, 1098 XH Amsterdam, The Netherlands Received June XX, 2017; accepted YYY ABSTRACT Context. The influence of stellar multiplicity on planet formation is not yet well determined. Most planets are found using indirect detection methods via the small radial velocity or photometric variations of the primary star. These indirect detection methods are not sensitive to wide stellar companions. High-resolution imaging is thus needed to identify potential (sub)stellar companions to these stars. Aims. In this study we aim to determine the (sub)stellar multiplicity status of exoplanet host stars, that were not previously investigated for stellar multiplicity in the literature. For systems with non-detections we provide detailed detection limits to make them accessible for further statistical analysis. Methods. For this purpose we have employed previously unpublished high-resolution imaging data taken with VLT/NACO in a wide variety of different scientific programs and publicly accessible in the ESO archive. We used astrometric and theoretical population synthesis to determine whether detected companion candidates are likely to be bound or are merely chance-projected background objects. Results. We provide detailed detection limits for 39 systems and investigate 29 previously unknown companion candidates around five systems.
    [Show full text]
  • TRUE MASSES of RADIAL-VELOCITY EXOPLANETS Robert A
    APP Template V1.01 Article id: apj513330 Typesetter: MPS Date received by MPS: 19/05/2015 PE: CE : LE: UNCORRECTED PROOF The Astrophysical Journal, 00:000000 (28pp), 2015 Month Day © 2015. The American Astronomical Society. All rights reserved. TRUE MASSES OF RADIAL-VELOCITY EXOPLANETS Robert A. Brown Space Telescope Science Institute, USA; [email protected] Received 2015 January 12; accepted 2015 April 14; published 2015 MM DD ABSTRACT We study the task of estimating the true masses of known radial-velocity (RV) exoplanets by means of direct astrometry on coronagraphic images to measure the apparent separation between exoplanet and host star. Initially, we assume perfect knowledge of the RV orbital parameters and that all errors are due to photon statistics. We construct design reference missions for four missions currently under study at NASA: EXO-S and WFIRST-S, with external star shades for starlight suppression, EXO-C and WFIRST-C, with internal coronagraphs. These DRMs reveal extreme scheduling constraints due to the combination of solar and anti-solar pointing restrictions, photometric and obscurational completeness, image blurring due to orbital motion, and the “nodal effect,” which is the independence of apparent separation and inclination when the planet crosses the plane of the sky through the host star. Next, we address the issue of nonzero uncertainties in RV orbital parameters by investigating their impact on the observations of 21 single-planet systems. Except for two—GJ 676 A b and 16 Cyg B b, which are observable only by the star-shade missions—we find that current uncertainties in orbital parameters generally prevent accurate, unbiased estimation of true planetary mass.
    [Show full text]
  • Archival VLT/Naco Multiplicity Investigation of Exoplanet Host Stars
    A&A 620, A102 (2018) Astronomy https://doi.org/10.1051/0004-6361/201731341 & c ESO 2018 Astrophysics Archival VLT/NaCo multiplicity investigation of exoplanet host stars J. Dietrich1,2 and C. Ginski1,3 1 Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands e-mail: [email protected] 2 Harvard University, Cambridge, MA 02138, USA 3 Anton Pannekoek Institute for Astronomy, University of Amsterdam, Science Park 904, 1098 XH Amsterdam, The Netherlands Received 9 June 2017 / Accepted 27 June 2018 ABSTRACT Context. The influence of stellar multiplicity on planet formation is not yet well determined. Most planets are found using indirect detection methods via the small radial velocity or photometric variations of the primary star. These indirect detection methods are not sensitive to wide stellar companions. High-resolution imaging is thus needed to identify potential (sub)stellar companions to these stars. Aims. In this study we aim to determine the (sub)stellar multiplicity status of exoplanet host stars, that were not previously investigated for stellar multiplicity in the literature. For systems with non-detections we provide detailed detection limits to make them accessible for further statistical analysis. Methods. For this purpose we have employed previously unpublished high-resolution imaging data taken with VLT/NACO in a wide variety of different scientific programs and publicly accessible in the ESO archive. We used astrometric and theoretical population synthesis to determine whether detected companion candidates are likely to be bound or are merely chance-projected background objects. Results. We provide detailed detection limits for 39 systems and investigate 29 previously unknown companion candidates around five systems.
    [Show full text]
  • Determining the True Mass of Radial-Velocity Exoplanets with Gaia 9 Planet Candidates in the Brown-Dwarf/Stellar Regime and 27 Confirmed Planets
    Astronomy & Astrophysics manuscript no. exoplanet_mass_gaia c ESO 2020 September 30, 2020 Determining the true mass of radial-velocity exoplanets with Gaia 9 planet candidates in the brown-dwarf/stellar regime and 27 confirmed planets F. Kiefer1; 2, G. Hébrard1; 3, A. Lecavelier des Etangs1, E. Martioli1; 4, S. Dalal1, and A. Vidal-Madjar1 1 Institut d’Astrophysique de Paris, Sorbonne Université, CNRS, UMR 7095, 98 bis bd Arago, 75014 Paris, France 2 LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université de Paris, 5 place Jules Janssen, 92195 Meudon, France? 3 Observatoire de Haute-Provence, CNRS, Universiteé d’Aix-Marseille, 04870 Saint-Michel-l’Observatoire, France 4 Laboratório Nacional de Astrofísica, Rua Estados Unidos 154, 37504-364, Itajubá - MG, Brazil Submitted on 2020/08/20 ; Accepted for publication on 2020/09/24 ABSTRACT Mass is one of the most important parameters for determining the true nature of an astronomical object. Yet, many published exoplan- ets lack a measurement of their true mass, in particular those detected thanks to radial velocity (RV) variations of their host star. For those, only the minimum mass, or m sin i, is known, owing to the insensitivity of RVs to the inclination of the detected orbit compared to the plane-of-the-sky. The mass that is given in database is generally that of an assumed edge-on system (∼90◦), but many other inclinations are possible, even extreme values closer to 0◦ (face-on). In such case, the mass of the published object could be strongly underestimated by up to two orders of magnitude.
    [Show full text]
  • Jupiter Analogs Orbit Stars with an Average Metallicity Close to That of the Sun
    Downloaded from orbit.dtu.dk on: Oct 05, 2021 Jupiter Analogs Orbit Stars with an Average Metallicity Close to That of the Sun Buchhave, Lars A.; Bitsch, Bertram; Johansen, Anders; Latham, David W.; Bizzarro, Martin; Bieryla, Allyson; Kipping, David M. Published in: Astrophysical Journal Link to article, DOI: 10.3847/1538-4357/aaafca Publication date: 2018 Document Version Publisher's PDF, also known as Version of record Link back to DTU Orbit Citation (APA): Buchhave, L. A., Bitsch, B., Johansen, A., Latham, D. W., Bizzarro, M., Bieryla, A., & Kipping, D. M. (2018). Jupiter Analogs Orbit Stars with an Average Metallicity Close to That of the Sun. Astrophysical Journal, 856(1), [37]. https://doi.org/10.3847/1538-4357/aaafca General rights Copyright and moral rights for the publications made accessible in the public portal are retained by the authors and/or other copyright owners and it is a condition of accessing publications that users recognise and abide by the legal requirements associated with these rights. Users may download and print one copy of any publication from the public portal for the purpose of private study or research. You may not further distribute the material or use it for any profit-making activity or commercial gain You may freely distribute the URL identifying the publication in the public portal If you believe that this document breaches copyright please contact us providing details, and we will remove access to the work immediately and investigate your claim. The Astrophysical Journal, 856:37 (11pp), 2018 March 20 https://doi.org/10.3847/1538-4357/aaafca © 2018.
    [Show full text]
  • Paul Robertson, Ph.D
    Paul Robertson, Ph.D. Assistant Professor Department of Physics & Astronomy Email: [email protected] The University of California, Irvine Phone: (949) 824-6660 4129 Frederick Reines Hall Web: http://faculty.sites.uci.edu/robertson/ Irvine, CA 92697 EDUCATION Doctor in Astrophysics, 2013 The University of Texas, Austin, TX Dissertation: “Discovering New Solar Systems: Jupiter Analogs and the Quest to Find Another Earth” Master of Arts in Astrophysics, 2010 The University of Texas, Austin, TX Thesis: “The Hobby-Eberly Telescope M dwarf Planet Search Program: New Observations and Results” Bachelor of Arts in Physics and Mathematics, 2008 The University of North Carolina, Chapel Hill, NC PROFESSIONAL APPOINTMENTS Assistant Professor, UC Irvine 2018-present NASA Sagan Fellow, Penn State University 2015-2017 Postdoctoral Fellow, Penn State University 2013-2015 AWARDS University of New South Wales Science Visiting Fellowship, 2016 Carl Sagan Fellowship, NASA, 2015 Graduate Continuing Fellowship, University of Texas, 2012-2013 Frank N. Edmonds Jr. Memorial Fellowship in Astronomy, The University of Texas, 2011-2012 Graduate with Distinction, The University of North Carolina, 2008 FIRST-AUTHORED PEER REVIEWED PUBLICATIONS Robertson, P., Anderson, T., Stefansson, G. et al. 2019, “Ultra-Stable Environment Control for the NEID Spectrometer: Design and Performance Demonstration.” Journal of Astronomical Telescopes, Instruments, and Systems, accepted. arXiv:1902.07729. Robertson, P. 2018. “Aliasing in the Radial Velocities of YZ Ceti: An Ultra-short Period for YZ Ceti c?” The Astrophysical Journal Letters, Vol. 864, p. 28. Robertson, P., Bender, C., Mahadevan, S., Roy, A., & Ramsey, L. W. 2016. “Proxima Centauri as a Benchmark for Stellar Activity Indicators in the Near Infrared.” The Astrophysical Journal, Vol.
    [Show full text]