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303 - 306 Poster Publ. Astron. Obs. Belgrade No. 98 (2018), 303 - 306 Poster SEARCH FOR POSSIBLE EXOMOONS WITH FAST TELESCOPE D. V. LUKIC¶ Institute of Physics, University of Belgrade, P.O. Box 57, 11001 Belgrade, Serbia E{mail: [email protected] Abstract. Our knowledge of the Solar System, encourage us to beleive that we might expect exomoons to be present around some of the known exoplanets. With present hardware we shall not be able to ¯nd exomoons with existing optical astronomy methods at least 10 years from now and even then, it will be hard task to detect them. We suggest radio astronomy based methods to search for possible exomoons around these exoplanets. Using data from the Exoplanet Orbit Database (EOD) we ¯nd 2 stars with Jovian exoplanets within 50 light years fully accessible by the new radio telescope, The Five-hundred-meter Aperture Spherical radio Telescope (FAST). 1. INTRODUCTION Discovery of the 51 Pegasi b (Mayor & Queloz 1995), exoplanet orbiting the Sun-like Main Sequence star, was only the ¯rst in the series of many exoplanets discovered thenceforth. The progress is made thanks to advanced detection techniques and instrumentation. Nowadays, the result is hundreds of con¯rmed and thousands of po- tential exoplanets, the most of them identi¯ed by the NASAs Kepler space telescope. Every prudent connoisseur of the Solar System would expect the presence of the exo- moons close to the known exoplanets. The Solar System's planets and dwarf planets are known to be orbited by 182 natural satellites. In our solar system, Jovian planets have the biggest collections of moons and we expect similar position for gas giants planets in extrasolar systems. Nonetheless, contemporary techniques for observation haven't made a single detection of any exomoon so far. One of the leading models de- scribing planetary satellites formation is the actively supplied gaseous accretion disk model (Canup & Ward 2006). In this model, the ¯nal total mass of satellite system, ¡4 approximately 10 MP (MP mass of planet) is given by a balance of the supply of material to the satellites, and satellite loss through orbital decay driven by the gas. 2. SELECTION OF DATA AND METHOD OF ANALYSIS Many of the detected exoplanets are the gas giants located in the habitable zone of their stars. These big planets cannot support life, but it is believed that some of their exomoons could be habitable. In our analysis, assuming that scaling law (Canup & Ward 2006) observed in the solar system also applies for extrasolar super- Jupiters (Heller & Pudritz 2014), we used planet's data from the Exoplanet Orbit 303 D. V. LUKIC¶ Database catalog (Wright et al. 2011 and Han et al 2014). We selected only exoplanets closer than 50 light years which have comparable mass or are more massive than Jupiter within declination limits of full sensitivity of new radio telescope in China. Approximately a half of them are hot or warm Jupiters. According to (Heller & Pudritz 2015) if these planets migrated in to the stellar habitable zones from beyond a few AU, they could be orbited by large, water rich satellites. The liquid water on surfaceDa istab possiblease catalo ong (W su±cientlyright et al. 2 massive011 and H satellites.an et al 2014). We selected only exoplanets closer than 50 light years which have comparable mass or are more massive than BesidesJupiter telescopeswithin decli explainednation limit ins of (Griessmeierfull sensitivity etof al.new 2011,radio t Noyolaelescope 2015)in Chin wea. have additionalApprox radioimatel telescopey a half of inthe ¯nalm are phasehot or ofwa construction,rm Jupiters. Ac Thecordin Five-hundred-meterg to (Heller & AperturePudr Sphericalitz 2015) if t radiohese p Telescopelanets migra (FAST)ted in to t (Nanhe stel etlar al.habi 2011)table zo andnes f latterrom be SKAyond tele- scope.a f FASTew AU, isthe locatedy could b ate o arbi greatted by depressionlarge, water withrich sa ate diameterllites. The ofliqu aboutid wate 800r on m at 25o.647Nsurfa andce is p 106ossoib.856E,le on su nearfficien thetly m villageassive s ofate Dawodang,llites. in Guizhou Province. FAST will be capableBesides oftel coveringescopes ex theplain skywithined in (Grie 40ssmo efromier et theal. zenith2011, N withoyola full2015 sensitivity.) we have Set of ninead receiversditional ra coversdio teles aco frequencype in final rangephase o fromf cons 70tru MHzction, toTh 3e F GHz.ive-hu Itndr hased-m aneter illumi- Aperture Spherical radio Telescope (FAST) (Nan et al. 2011) and latter SKA tele- natedsc apertureope. FAS ofT i 300s loca mted diameter.at a great FASTdepressi ison anwit orderh a dia ofme magnitudeter of about more800 m sensitiveat than 100-m25o.647N telescopesand 106o.8 at56 GreenE, near Bank,the villa USA,ge of D andawo E®elsberg,dang, in Guiz Germanyhou Provin andce. F aboutAST two timesw moreill be thancapabl Giante of cov Meterwaveering the skyw Radioithin 4 Telescope0o from the (GMRT),zenith with India.full sensitivity. Set Weof countnine re onceiv interactioners covers a f ofreq magneticuency rang ¯elde from of7 extrasolar0 MHz to 3 planetsGHz. It withhas a plasmasn illumi- from exomoonsnated (Zarkaapertur 2007).e of 300 Inm Solardiame system,ter. FAS e.g.T is thean particlesorder of m fromagnitu Io'sde m volcanicore sensi eruptionstive than 100-m telescopes at Green Bank, USA, and Effelsberg, Germany and about two interact with the Jupiter's magnetosphere to produce intense decameter radio waves. times more than Giant Meterwave Radio Telescope (GMRT), India. From the ground, these radio waves are detectable in the frequency range from 10 to We count on interaction of magnetic field of extrasolar planets with plasmas from 40 MHzexom (Zarkaoons (Z 1998).arka 200 The7). In generationSolar system mechanism, e.g. the parti iscle thes from cyclotron-maserIo's volcanic erup instabilitytions (Wu etinte al.ract 1979).with the ListedJupiter's frequenciesmagnetosphe inre t Tableo produ 1ce areinte maximumnse decamete valuesr radio reportedwaves. in (GriessmeieretFrom the gr al.ound 2007)., these ra Indio Tablewaves a 2re wedetec comparetable in th frequenciese frequency rafnmGge frcalculatedom 10 to by (Griessmeier40 MHz et(Za al.rka 2007),1998). withThe g otherenerati modelson mecha ofnis extrasolarm is the cyc planetslotron-m radioaser in emissionstability fmL (Wu et al. 1979). Listed frequencies in Table 1 are maximum values reported in (Lazio et al. 2004) and fmR (Reiners & Christiansen 2010) and expected radio fluxes. Other(G radioriessm telescopeseieret al. 2 with007). theIn T mostable 2 suitablewe comp frequencyare frequenc rangeies fmG are:calc superulated b LOFARy (Griessmeier et al. 2007), with other models of extrasolar planets radio emission fmL extension(Lazio (NenuFAR,et al. 2004) a 10-80nd f MHz)(Reiner ins & France,Christian 1-2senmJy2010) aatnd 4MHzexpecte bandwidth,d radio fluxes. Giant mR 0:5 MeterwaveOther Radioradio te Telescopelescopes wit (GMRT,h the mos 153t suit MHz)able fre inqu India,ency ra 0.2nge mJy=are: su(pt=er15LminutesOFAR ) in a 4e MHzxtensio bandwith,n (NenuFAR and, 10 Ukrainian-80 MHz) in T-shapedFrance, 1- Radio2 mJy telescopeat 4MHz b (UTR-2,andwidth, 8-40Giant MHz). Meterwave Radio Telescope (GMRT, 153 MHz) in India, 0.2 mJy=(t=15minutes)0:5 in a 4 MHz bandwith, andTableUkrain 1.ianPossibleT-shaped exomoons.Radio telescope (UTR-2, 8-40 MHz). Table 1. Possible exomoons P lan etN ame M ass S tar type S emimajor D istan ce S atellite D eclin ation F requ ency A x is [p c] mass o 0 00 ep s E rid ani b 1.55 M J K 2V 3.4 A U 3.22 0.049 M ⊕ -09 27 29.7312 33.2 M H z o 0 00 G liese 876 b 2.27 M J M 4V 0.2 A U 4.69 0.072 M ⊕ -14 15 49.32 38.2 M H z o 0 00 G liese 876 c 0.7 M J M 4V 0.13 A U 4.69 0.022 M ⊕ -14 15 49.32 16.4 M H z o 0 00 G liese 849 b 0.91 M J M 3.5V 2.39 A U 9.1 0.0289 M ⊕ -4 38 26.62 21.8 M H z o 0 00 G liese 849 c 0.94 M J M 3.5V 4.82 A U 9.1 0.0298 M ⊕ -4 38 26.62 o 0 00 H D 62509 b 2.9 M J K 0III 1.64 A U 10.3 0.092 M ⊕ + 28 01 35 49.5 M H z o 0 00 55 C nc b 0.8 M J G 8V 0.11 A U 12.3 0.025 M ⊕ + 28 19 51 18.9 M H z o 0 00 55 C nc d 3.878 M J G 8V 5.74 A U 12.3 0.123 M ⊕ + 28 19 51 61.4 M H z o 0 00 H D 147513 b 1.21 M J G 1V H -04 1.32 A U 12.9 0.038 M ⊕ + 39 11 34.7121 24.5 M H z o 0 00 u p s A nd A b 0.62 M J F 8V 0.059 A U 13.47 0.019 M ⊕ + 41 24 19.6443 2.4 M H z o 0 00 u p s A nd A c 13.98 M J F 8V 0.832 A U 13.47 0.44 M ⊕ + 41 24 19.6443 38.4 M H z o 0 00 u p s A nd A d 10.25 M J F 8V 2.53 A U 13.47 0.33 M ⊕ + 41 24 19.6443 61.4 M H z o 0 00 u p s A nd A e 0.96 M J F 8V 5.25 A U 13.470 0.031 M ⊕ + 41 24 19.6443 o 0 00 47 U M a b 2.5 M J G 1V 2.1 A U 14.06 0.079 M ⊕ + 40 25 27.97 46.6 M H z o 0 00 H IP 79431 b 2.00 M J M 3V 0.36 A U 14.4 0.064 M ⊕ -18 52 31.8 40 M H z o 0 00 H D 176051 b 1.5 M J F 9V 1.76 A U 15 0.047 M ⊕ + 32 54 5 A selected planets are presented in Table 1.
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