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E. Plávalová 1,2 1 Dpt The UK Community Exoplanet Conference 2015, Warwick , 30 March ̶ 01 April 2015 Do we need a system of classification for extrasolar planets? E. Plávalová 1,2 1 Dpt. of astronomy, Earth's physics and meteorology, Comenius University, Bratislava, [email protected] 2 Astronomical Institute of the Slovak Academy of Sciences, Bratislava Abstract Spectral classification of stars is now common and widely used. Only a few people know that its evolution into today's form has taken a matter of decades and that in its infancy was the subject of ridicule. This year is the 20th anniversary of the discovery of the first extrasolar planet 51Peg b. Almost two thousand planets and thousands of planet-candidates have been discovered since then. Isn't it high time to start talking about a system of classification? Every day new planet-candidates are being discovered and with the volume of planets expected to dramatically accelerate, without a good system of classification in place, the backlog of planets waiting to be analyzed would slow down research dramatically. We can discuss how this classification (taxonomy) should look like and be presented according to the existing system of classification published by Plávalová (2012). This classification uses four main parameters which cover the mass, semi-major axis, temperature, eccentricity, plus one optional parameter which is not always known. A brief history of classification System of classification of extrasolar planets Stellar classification Planet classification Mass of the EPs Semi-major axis (Units of the mass) 1814 1969 distance from its parent star (semi- M– less than 0.002 MJup major axis) described in logarithm Joseph Fraunhofer invented the Peter Van de Kamp [15] reported a periodic 9E – from 0.002 to 0.03 M with a base 10 spectroscope and was the first to "wobble" in Barnard star’s motion, apparently due Jup N – from 0.03 to 0.6 MJup e.g.: observe solar and stellar spectra. to planetary companions. In 1973 astronomers J – from 0.6 to 5 MJup for Earth it is 0 George Gatewood and Heinrich Eichhorn [4], 1862 S – from 5 to15 MJup for Mercury it is -0.4 using data obtained with improved equipment on D – more than 15 MJup for semi-major axis 0.05 AU is -1.3 Lewis Morris Rutherfurd amassed the 30-inch Thaw Refractor telescope, did not sufficient spectra to attempt the detect any planets but instead detected a change classification of stars into three in the colour-dependent image scale of the images M0.2W1t (Mars) groups. Modern equivalent groups obtained from by Van de Kamp. would be the late-type stars, the late- B to early-F stars, and the OB stars. 1988 Mean Dyson temperature (K) Bruce Campbell, Gordon A.H. Walker, and 1860-1870 (Mean Orbit temperature) Stephenson Yang reported an interesting Pietro Angelo Secchi classified the spectra of stars phenomenon [2]; the radial velocity variations of F – to 250 K into two classes, basically the early I and the late- binary star γCephei, seemed to suggest the W – from 250 to 450 K Eccentricity Surface attribute G – from 450 to 1000 K types II. In 1866 he added what are existence of a Jupiter-like planet around one of used to only the first decimal t – Terrestrial planet R – higher than 1000 K now the M-types III, and two years the stars, but by 1992 had changed their minds position of the value of g – Gaseous planet P – pulsar class later he identified some faint red [14]. However, by 2003, Hatzes et al. [6] eccentricity, which is rounded i – Ice planet stars as type IV, the carbon stars. confirmed the existence of the planet around Later yet he felt compelled to γCephei. separate some emission-line stars Figure 1: Schematic explanation - a definition of the taxonomy of the planets for which we are able to 1991 into a further class, V. determine the taxonomy scale. 1881-1890 Andrew Geoffrey Lyne announced the first ever pulsar planet discovered around PSR 1829-10 [1]. How it works? Examples Williamina Fleming classified more than 10,000 However, this was later retracted, just before the star. It used a scheme in which the previously first real pulsar planets were announced. This system uses four abbreviated parameters, The code for Earth is E0W0t, for Uranus N1.3F0i used Secchi classes (I to IV) were written as a code, to allow for rapid recognition and for 55 Cnc e is E-1.8R1. In practise, using the 1992 of a planet’s characteristics. divided into more specific classes, whole code is sometimes unnecessary. Then we given letters from A to N. Also, the Aleksander Wolszczan and Dale Frail announced The first parameter takes the form of the units of letters O, P and Q were used, O for the discovery of a multi-planet planetary system can use a minimal code which for example could the mass, where M is less than 0.002 MJup and contain only the units of mass with the MDT, for stars whose spectra consisted mainly around the millisecond pulsar PSR 1257+12 [16]. roughly represents the mass of Mercury, E is a of bright lines, P for planetary example, Earth could be written as EW, 55 Cnc e 1995 mass from 0.002 to 0.03 MJup (roughly the mass nebulae, and Q for stars not fitting of Earth), N is a mass from 0.03 to 0.6 MJup as ER and Uranus as NF. The first exoplanet to be discovered which orbits a into any other class. (roughly the mass of Neptune), J is a mass from main sequence star, 51 Peg b, was discovered by Classifica- 0.6 to 5 MJup (roughly the mass of Jupiter), S is a Around 1890 Michel Mayor and Didier Queloz [9]. Planet Minimal code mass from 5 to 15 MJup (Super Jupiter) and unit tion code Joseph Norman Lockyer offered his own spectral 2003 D is for planets with a mass more than 15 MJup . classification scheme. The differentiation of stars Solar system into ascending and descending David Sudarsky, Adam Burrows, and Ivan The second parameter is the planet’s distance Mercury M-0.4G2t MG temperature branches was based on Hubeny created the so called Sudarsky's from its parent star (semi-major axis) described Venus E-0.1G0t EG his “meteoritic hypothesis” for the classification [13] of extrasolar gas giant planets, in logarithm with base 10. for the purpose of predicting their appearance Earth E0W0t EW origin and subsequent evolution of The third parameter is the Mean Dyson based on their temperature. Gas giants are split stars. His classifications were never Temperature (MDT) of the planet, for which we Mars M0.2W1t MW into five classes (numbered using Roman generally accepted, he did at least established four main temperature classes numerals) according to their modelled physical Jupiter J0.7F0g JF distinguish the spectra of giants and according to the state phase of water; F atmospheric properties. Saturn supergiants. represents the Freezing class, W the Water Class, N1F1g NF 1895 2007 G the Gaseous Class, and R the Roasters Class. Uranus N1.3F0i NF We devised one additional class, however, P Hermann Carl Vogel combined Simone Marchi [8] used as many inputs as Neptune N1.5F0i NF representing the Pulsar Class, which concerns Secchi’s classes III and IV, since they possible for the analysis, in particular the extrasolar planets orbiting pulsar stars. The Planets orbiting 55 Cnc were both based on broad bands, and planetary mass, semi-major axis, eccentricity, Dyson temperature is a temperature that has an went on to subdivide the resulting stellar mass and stellar metallicity. He identify the 55 Cnc b J-0.9R0 JR artificial sphere the size of a planetary orbit three classes. However, the discovery best procedure to follow: a multivariate statistical 55 Cnc c N-0.6G1 NG (Dyson sphere) [3]. The MDT is the arithmetical of helium both in stars and on earth analysis (PCA) to find the most important mean of the Dyson temperature taken from 10 55 Cnc d J0.8F0 JF was to revise his scheme, subdividing variables, and then hierarchical cluster analysis. equal segments, according to the second his class Ia. His best solution consists of five clusters. 55 Cnc e E-1.8R1 ER Keplerian law. 1897 2009 55 Cnc f N-0.1W0 NW The fourth parameter is eccentricity, where we An amateur astronomer, Sir Francis Kennedy Lundock et al. [7] had acquired spectra for all of used only the first rounded decimal position for Miscellaneous extrasolar planets McClean’s spectral classification the solar system planets and many smaller bodies its value. Many extrasolar planets were published 11 Com b D0.1R2 DR system was able from the beginning using TRISPEC. The spectra are divided by their without a known value for their eccentricity, and 14 And b S-0.1R0 SR to include the stars with neutral characteristic shapes into three distinct groups: then the classification code is written without a helium absorption. It was modelled gas planets, soil planets, and ice planets. Venus fourth parameter. 75 Cet b J0.3G JG on Secchi’s, with Vogel-like represents a fourth possible group. If the attributes of the surface of the planet are Kepler 9b N-0.8R1 NR revisions, and his groups 2012 known, we are able to establish a fifth additional corresponded to the MK series of B, Kepler 9c N-0.6G1 NG parameter where t represents a terrestrial planet, A, F, G-K, M, and carbon stars. Eva Plávalová [12] proposed an extrasolar planet CoRoT-9 b J-0.4G1 JG taxonomy scale with four main parameters which g a gaseous planet, or i an ice planet.
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