Discovery of a cool planet of 5.5 earth masses through gravitational microlensing
Identifieur interne : 004461 ( PascalFrancis/Corpus ); précédent : 004460; suivant : 004462Discovery of a cool planet of 5.5 earth masses through gravitational microlensing
Auteurs : J.-P. Beaulieu ; D. P. Bennett ; P. Fouque ; A. Williams ; M. Dominik ; U. G. J Rgensen ; D. Kubas ; A. Cassan ; C. Coutures ; J. Greenhill ; K. Hill ; J. Menzies ; P. D. Sackett ; M. Albrow ; S. Brillant ; J. A. R. Caldwell ; J. J. Calitz ; K. H. Cook ; E. Corrales ; M. Desort ; S. Dieters ; D. Dominis ; J. Donatowicz ; M. Hoffman ; S. Kane ; J.-B. Marquette ; R. Martin ; P. Meintjes ; K. Pollard ; K. Sahu ; C. Vinter ; J. Wambsganss ; K. Woller ; K. Horne ; I. Steele ; D. M. Bramich ; M. Burgdorf ; C. Snodgrass ; M. Bode ; A. Udalski ; M. K. Szymanski ; M. Kubiak ; T. Wieckowski ; G. Pietrzynski ; I. Soszynski ; O. Szewczyk ; T. Wyrzykowski ; B. Paczynski ; F. Abe ; I. A. Bond ; T. R. Britton ; A. C. Gilmore ; J. B. Hearnshaw ; Y. Itow ; K. Kamiya ; P. M. Kilmartin ; A. V. Korpela ; K. Masuda ; Y. Matsubara ; M. MotomuraSource :
- Nature : (London) [ 0028-0836 ] ; 2006.
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Abstract
In the favoured core-accretion model of formation of planetary systems, solid planetesimals accumulate to build up planetary cores, which then accrete nebular gas if they are sufficiently massive. Around M-dwarf stars (the most common stars in our Galaxy), this model favours the formation of Earth-mass (M◦+) to Neptune-mass planets with orbital radii of 1 to 10 astronomical units (AU), which is consistent with the small number of gas giant planets known to orbit M-dwarf host stars1-4. More than 170 extrasolar planets have been discovered with a wide range of masses and orbital periods, but planets of Neptune's mass or less have not hitherto been detected at separations of more than 0.15 AU from normal stars. Here we report the discovery of a 5.5+5.5-2.7M◦+ planetary companion at a separation of 2.6+1.5-0.6AU from a 0.22+0.21-0.11 M◦. M-dwarf star, where M◦. refers to a solar mass. (We propose to name it OGLE-2005-BLG-390Lb, indicating a planetary mass companion to the lens star of the microlensing event.) The mass is lower than that of GJ876d (ref. 5), although the error bars overlap. Our detection suggests that such cool, sub-Neptune-mass planets may be more common than gas giant planets, as predicted by the core accretion theory.
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Format Inist (serveur)
| NO : | PASCAL 06-0192157 INIST |
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| ET : | Discovery of a cool planet of 5.5 earth masses through gravitational microlensing |
| AU : | BEAULIEU (J.-P.); BENNETT (D. P.); FOUQUE (P.); WILLIAMS (A.); DOMINIK (M.); JØRGENSEN (U. G.); KUBAS (D.); CASSAN (A.); COUTURES (C.); GREENHILL (J.); HILL (K.); MENZIES (J.); SACKETT (P. D.); ALBROW (M.); BRILLANT (S.); CALDWELL (J. A. R.); CALITZ (J. J.); COOK (K. H.); CORRALES (E.); DESORT (M.); DIETERS (S.); DOMINIS (D.); DONATOWICZ (J.); HOFFMAN (M.); KANE (S.); MARQUETTE (J.-B.); MARTIN (R.); MEINTJES (P.); POLLARD (K.); SAHU (K.); VINTER (C.); WAMBSGANSS (J.); WOLLER (K.); HORNE (K.); STEELE (I.); BRAMICH (D. M.); BURGDORF (M.); SNODGRASS (C.); BODE (M.); UDALSKI (A.); SZYMANSKI (M. K.); KUBIAK (M.); WIECKOWSKI (T.); PIETRZYNSKI (G.); SOSZYNSKI (I.); SZEWCZYK (O.); WYRZYKOWSKI (T.); PACZYNSKI (B.); ABE (F.); BOND (I. A.); BRITTON (T. R.); GILMORE (A. C.); HEARNSHAW (J. B.); ITOW (Y.); KAMIYA (K.); KILMARTIN (P. M.); KORPELA (A. V.); MASUDA (K.); MATSUBARA (Y.); MOTOMURA (M.) |
| AF : | PLANET/RoboNet Collaboration/France (1 aut., 2 aut., 3 aut., 4 aut., 5 aut., 6 aut., 7 aut., 8 aut., 9 aut., 10 aut., 11 aut., 12 aut., 13 aut., 14 aut., 15 aut., 16 aut., 17 aut., 18 aut., 19 aut., 20 aut.); Institut d'Astrophysique de Paris, CNRS, Université Pierre et Marie Curie UMR7095, 98bis Boulevard Arago/75014 Pans/France (1 aut., 8 aut., 19 aut., 20 aut., 26 aut.); MOA Collaboration/Macao (2 aut., 49 aut., 50 aut., 51 aut., 52 aut., 53 aut., 54 aut., 55 aut., 56 aut., 57 aut., 58 aut., 59 aut., 60 aut.); University of Notre Dame, Department of Physics/Notre Dame, Indiana 46556-5670/Etats-Unis (2 aut.); Observatoire Midi-Pyrénées, Laboratoire d'Astrophysique, UMR 5572, Université Paul Sabatier-Toulouse 3,14 avenue Edouard Belin/31400 Toulouse/France (3 aut.); Perth Observatory, Walnut Road/Bickley, Perth, WA 6076/Australie (4 aut., 27 aut.); Scottish Universities Physics Alliance, University of St Andrews, School of Physics and Astronomy/North Haugh, St Andrews KY16 9SS/Royaume-Uni (5 aut., 34 aut., 36 aut.); Niels Bohr Institutet, Astronomisk Observatorium, Juliane Manes Vej 30/2100 København/Danemark (6 aut., 31 aut., 33 aut.); European Southern Observatory/Casilla 19001, Santiago 19/Chili (7 aut., 15 aut.); CEA DAPNIA/SPP Saclay/91191 Gif-sur-Yvette/France (9 aut.) |
| DT : | Publication en série; Niveau analytique |
| SO : | Nature : (London); ISSN 0028-0836; Coden NATUAS; Royaume-Uni; Da. 2006; Vol. 439; No. 7075; Pp. 437-440; Bibl. 30 ref. |
| LA : | Anglais |
| EA : | In the favoured core-accretion model of formation of planetary systems, solid planetesimals accumulate to build up planetary cores, which then accrete nebular gas if they are sufficiently massive. Around M-dwarf stars (the most common stars in our Galaxy), this model favours the formation of Earth-mass (M◦+) to Neptune-mass planets with orbital radii of 1 to 10 astronomical units (AU), which is consistent with the small number of gas giant planets known to orbit M-dwarf host stars1-4. More than 170 extrasolar planets have been discovered with a wide range of masses and orbital periods, but planets of Neptune's mass or less have not hitherto been detected at separations of more than 0.15 AU from normal stars. Here we report the discovery of a 5.5+5.5-2.7M◦+ planetary companion at a separation of 2.6+1.5-0.6AU from a 0.22+0.21-0.11 M◦. M-dwarf star, where M◦. refers to a solar mass. (We propose to name it OGLE-2005-BLG-390Lb, indicating a planetary mass companion to the lens star of the microlensing event.) The mass is lower than that of GJ876d (ref. 5), although the error bars overlap. Our detection suggests that such cool, sub-Neptune-mass planets may be more common than gas giant planets, as predicted by the core accretion theory. |
| CC : | 001E03C82C |
| FD : | Microlentille; Accrétion; Modèle; Cosmogonie planétaire; Planétésimales; Noyau planétaire; Etoile M; Etoile naine; Planète géante; Orbite; Planète extrasolaire; Lentille gravitationnelle |
| ED : | Microlenses; Accretion; Models; Planetary cosmogony; Planetesimals; Planet core; M stars; Dwarf stars; Giant planet; Orbits; Extrasolar planets; Gravitational lenses |
| SD : | Modelo; Cosmogonía planetaria; Núcleo planetario; Planeta gigante |
| LO : | INIST-142.354000134741690160 |
| ID : | 06-0192157 |
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Pascal:06-0192157Le document en format XML
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Hill</name><affiliation><inist:fA14 i1="01"><s1>PLANET/RoboNet Collaboration</s1><s3>FRA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>9 aut.</sZ><sZ>10 aut.</sZ><sZ>11 aut.</sZ><sZ>12 aut.</sZ><sZ>13 aut.</sZ><sZ>14 aut.</sZ><sZ>15 aut.</sZ><sZ>16 aut.</sZ><sZ>17 aut.</sZ><sZ>18 aut.</sZ><sZ>19 aut.</sZ><sZ>20 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Menzies, J" sort="Menzies, J" uniqKey="Menzies J" first="J." last="Menzies">J. Menzies</name><affiliation><inist:fA14 i1="01"><s1>PLANET/RoboNet Collaboration</s1><s3>FRA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>9 aut.</sZ><sZ>10 aut.</sZ><sZ>11 aut.</sZ><sZ>12 aut.</sZ><sZ>13 aut.</sZ><sZ>14 aut.</sZ><sZ>15 aut.</sZ><sZ>16 aut.</sZ><sZ>17 aut.</sZ><sZ>18 aut.</sZ><sZ>19 aut.</sZ><sZ>20 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Sackett, P D" sort="Sackett, P D" uniqKey="Sackett P" first="P. D." last="Sackett">P. D. Sackett</name><affiliation><inist:fA14 i1="01"><s1>PLANET/RoboNet Collaboration</s1><s3>FRA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>9 aut.</sZ><sZ>10 aut.</sZ><sZ>11 aut.</sZ><sZ>12 aut.</sZ><sZ>13 aut.</sZ><sZ>14 aut.</sZ><sZ>15 aut.</sZ><sZ>16 aut.</sZ><sZ>17 aut.</sZ><sZ>18 aut.</sZ><sZ>19 aut.</sZ><sZ>20 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Albrow, M" sort="Albrow, M" uniqKey="Albrow M" first="M." last="Albrow">M. Albrow</name><affiliation><inist:fA14 i1="01"><s1>PLANET/RoboNet Collaboration</s1><s3>FRA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>9 aut.</sZ><sZ>10 aut.</sZ><sZ>11 aut.</sZ><sZ>12 aut.</sZ><sZ>13 aut.</sZ><sZ>14 aut.</sZ><sZ>15 aut.</sZ><sZ>16 aut.</sZ><sZ>17 aut.</sZ><sZ>18 aut.</sZ><sZ>19 aut.</sZ><sZ>20 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Brillant, S" sort="Brillant, S" uniqKey="Brillant S" first="S." last="Brillant">S. 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Vinter</name><affiliation><inist:fA14 i1="08"><s1>Niels Bohr Institutet, Astronomisk Observatorium, Juliane Manes Vej 30</s1><s2>2100 København</s2><s3>DNK</s3><sZ>6 aut.</sZ><sZ>31 aut.</sZ><sZ>33 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Wambsganss, J" sort="Wambsganss, J" uniqKey="Wambsganss J" first="J." last="Wambsganss">J. Wambsganss</name></author><author><name sortKey="Woller, K" sort="Woller, K" uniqKey="Woller K" first="K." last="Woller">K. Woller</name><affiliation><inist:fA14 i1="08"><s1>Niels Bohr Institutet, Astronomisk Observatorium, Juliane Manes Vej 30</s1><s2>2100 København</s2><s3>DNK</s3><sZ>6 aut.</sZ><sZ>31 aut.</sZ><sZ>33 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Horne, K" sort="Horne, K" uniqKey="Horne K" first="K." last="Horne">K. 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Desort</name><affiliation><inist:fA14 i1="01"><s1>PLANET/RoboNet Collaboration</s1><s3>FRA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>9 aut.</sZ><sZ>10 aut.</sZ><sZ>11 aut.</sZ><sZ>12 aut.</sZ><sZ>13 aut.</sZ><sZ>14 aut.</sZ><sZ>15 aut.</sZ><sZ>16 aut.</sZ><sZ>17 aut.</sZ><sZ>18 aut.</sZ><sZ>19 aut.</sZ><sZ>20 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="02"><s1>Institut d'Astrophysique de Paris, CNRS, Université Pierre et Marie Curie UMR7095, 98bis Boulevard Arago</s1><s2>75014 Pans</s2><s3>FRA</s3><sZ>1 aut.</sZ><sZ>8 aut.</sZ><sZ>19 aut.</sZ><sZ>20 aut.</sZ><sZ>26 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Dieters, S" sort="Dieters, S" uniqKey="Dieters S" first="S." last="Dieters">S. Dieters</name></author><author><name sortKey="Dominis, D" sort="Dominis, D" uniqKey="Dominis D" first="D." last="Dominis">D. 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Vinter</name><affiliation><inist:fA14 i1="08"><s1>Niels Bohr Institutet, Astronomisk Observatorium, Juliane Manes Vej 30</s1><s2>2100 København</s2><s3>DNK</s3><sZ>6 aut.</sZ><sZ>31 aut.</sZ><sZ>33 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Wambsganss, J" sort="Wambsganss, J" uniqKey="Wambsganss J" first="J." last="Wambsganss">J. Wambsganss</name></author><author><name sortKey="Woller, K" sort="Woller, K" uniqKey="Woller K" first="K." last="Woller">K. Woller</name><affiliation><inist:fA14 i1="08"><s1>Niels Bohr Institutet, Astronomisk Observatorium, Juliane Manes Vej 30</s1><s2>2100 København</s2><s3>DNK</s3><sZ>6 aut.</sZ><sZ>31 aut.</sZ><sZ>33 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Horne, K" sort="Horne, K" uniqKey="Horne K" first="K." last="Horne">K. Horne</name><affiliation><inist:fA14 i1="07"><s1>Scottish Universities Physics Alliance, University of St Andrews, School of Physics and Astronomy</s1><s2>North Haugh, St Andrews KY16 9SS</s2><s3>GBR</s3><sZ>5 aut.</sZ><sZ>34 aut.</sZ><sZ>36 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Steele, I" sort="Steele, I" uniqKey="Steele I" first="I." last="Steele">I. Steele</name></author><author><name sortKey="Bramich, D M" sort="Bramich, D M" uniqKey="Bramich D" first="D. M." last="Bramich">D. M. Bramich</name><affiliation><inist:fA14 i1="07"><s1>Scottish Universities Physics Alliance, University of St Andrews, School of Physics and Astronomy</s1><s2>North Haugh, St Andrews KY16 9SS</s2><s3>GBR</s3><sZ>5 aut.</sZ><sZ>34 aut.</sZ><sZ>36 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Burgdorf, M" sort="Burgdorf, M" uniqKey="Burgdorf M" first="M." last="Burgdorf">M. Burgdorf</name></author><author><name sortKey="Snodgrass, C" sort="Snodgrass, C" uniqKey="Snodgrass C" first="C." last="Snodgrass">C. Snodgrass</name></author><author><name sortKey="Bode, M" sort="Bode, M" uniqKey="Bode M" first="M." last="Bode">M. Bode</name></author><author><name sortKey="Udalski, A" sort="Udalski, A" uniqKey="Udalski A" first="A." last="Udalski">A. Udalski</name></author><author><name sortKey="Szymanski, M K" sort="Szymanski, M K" uniqKey="Szymanski M" first="M. K." last="Szymanski">M. K. Szymanski</name></author><author><name sortKey="Kubiak, M" sort="Kubiak, M" uniqKey="Kubiak M" first="M." last="Kubiak">M. Kubiak</name></author><author><name sortKey="Wieckowski, T" sort="Wieckowski, T" uniqKey="Wieckowski T" first="T." last="Wieckowski">T. Wieckowski</name></author><author><name sortKey="Pietrzynski, G" sort="Pietrzynski, G" uniqKey="Pietrzynski G" first="G." last="Pietrzynski">G. Pietrzynski</name></author><author><name sortKey="Soszynski, I" sort="Soszynski, I" uniqKey="Soszynski I" first="I." last="Soszynski">I. Soszynski</name></author><author><name sortKey="Szewczyk, O" sort="Szewczyk, O" uniqKey="Szewczyk O" first="O." last="Szewczyk">O. Szewczyk</name></author><author><name sortKey="Wyrzykowski, T" sort="Wyrzykowski, T" uniqKey="Wyrzykowski T" first="T." last="Wyrzykowski">T. Wyrzykowski</name></author><author><name sortKey="Paczynski, B" sort="Paczynski, B" uniqKey="Paczynski B" first="B." last="Paczynski">B. Paczynski</name></author><author><name sortKey="Abe, F" sort="Abe, F" uniqKey="Abe F" first="F." last="Abe">F. Abe</name><affiliation><inist:fA14 i1="03"><s1>MOA Collaboration</s1><s3>MAC</s3><sZ>2 aut.</sZ><sZ>49 aut.</sZ><sZ>50 aut.</sZ><sZ>51 aut.</sZ><sZ>52 aut.</sZ><sZ>53 aut.</sZ><sZ>54 aut.</sZ><sZ>55 aut.</sZ><sZ>56 aut.</sZ><sZ>57 aut.</sZ><sZ>58 aut.</sZ><sZ>59 aut.</sZ><sZ>60 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Bond, I A" sort="Bond, I A" uniqKey="Bond I" first="I. A." last="Bond">I. A. Bond</name><affiliation><inist:fA14 i1="03"><s1>MOA Collaboration</s1><s3>MAC</s3><sZ>2 aut.</sZ><sZ>49 aut.</sZ><sZ>50 aut.</sZ><sZ>51 aut.</sZ><sZ>52 aut.</sZ><sZ>53 aut.</sZ><sZ>54 aut.</sZ><sZ>55 aut.</sZ><sZ>56 aut.</sZ><sZ>57 aut.</sZ><sZ>58 aut.</sZ><sZ>59 aut.</sZ><sZ>60 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Britton, T R" sort="Britton, T R" uniqKey="Britton T" first="T. R." last="Britton">T. R. Britton</name><affiliation><inist:fA14 i1="03"><s1>MOA Collaboration</s1><s3>MAC</s3><sZ>2 aut.</sZ><sZ>49 aut.</sZ><sZ>50 aut.</sZ><sZ>51 aut.</sZ><sZ>52 aut.</sZ><sZ>53 aut.</sZ><sZ>54 aut.</sZ><sZ>55 aut.</sZ><sZ>56 aut.</sZ><sZ>57 aut.</sZ><sZ>58 aut.</sZ><sZ>59 aut.</sZ><sZ>60 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Gilmore, A C" sort="Gilmore, A C" uniqKey="Gilmore A" first="A. C." last="Gilmore">A. C. Gilmore</name><affiliation><inist:fA14 i1="03"><s1>MOA Collaboration</s1><s3>MAC</s3><sZ>2 aut.</sZ><sZ>49 aut.</sZ><sZ>50 aut.</sZ><sZ>51 aut.</sZ><sZ>52 aut.</sZ><sZ>53 aut.</sZ><sZ>54 aut.</sZ><sZ>55 aut.</sZ><sZ>56 aut.</sZ><sZ>57 aut.</sZ><sZ>58 aut.</sZ><sZ>59 aut.</sZ><sZ>60 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Hearnshaw, J B" sort="Hearnshaw, J B" uniqKey="Hearnshaw J" first="J. B." last="Hearnshaw">J. B. Hearnshaw</name><affiliation><inist:fA14 i1="03"><s1>MOA Collaboration</s1><s3>MAC</s3><sZ>2 aut.</sZ><sZ>49 aut.</sZ><sZ>50 aut.</sZ><sZ>51 aut.</sZ><sZ>52 aut.</sZ><sZ>53 aut.</sZ><sZ>54 aut.</sZ><sZ>55 aut.</sZ><sZ>56 aut.</sZ><sZ>57 aut.</sZ><sZ>58 aut.</sZ><sZ>59 aut.</sZ><sZ>60 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Itow, Y" sort="Itow, Y" uniqKey="Itow Y" first="Y." last="Itow">Y. Itow</name><affiliation><inist:fA14 i1="03"><s1>MOA Collaboration</s1><s3>MAC</s3><sZ>2 aut.</sZ><sZ>49 aut.</sZ><sZ>50 aut.</sZ><sZ>51 aut.</sZ><sZ>52 aut.</sZ><sZ>53 aut.</sZ><sZ>54 aut.</sZ><sZ>55 aut.</sZ><sZ>56 aut.</sZ><sZ>57 aut.</sZ><sZ>58 aut.</sZ><sZ>59 aut.</sZ><sZ>60 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Kamiya, K" sort="Kamiya, K" uniqKey="Kamiya K" first="K." last="Kamiya">K. Kamiya</name><affiliation><inist:fA14 i1="03"><s1>MOA Collaboration</s1><s3>MAC</s3><sZ>2 aut.</sZ><sZ>49 aut.</sZ><sZ>50 aut.</sZ><sZ>51 aut.</sZ><sZ>52 aut.</sZ><sZ>53 aut.</sZ><sZ>54 aut.</sZ><sZ>55 aut.</sZ><sZ>56 aut.</sZ><sZ>57 aut.</sZ><sZ>58 aut.</sZ><sZ>59 aut.</sZ><sZ>60 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Kilmartin, P M" sort="Kilmartin, P M" uniqKey="Kilmartin P" first="P. M." last="Kilmartin">P. M. Kilmartin</name><affiliation><inist:fA14 i1="03"><s1>MOA Collaboration</s1><s3>MAC</s3><sZ>2 aut.</sZ><sZ>49 aut.</sZ><sZ>50 aut.</sZ><sZ>51 aut.</sZ><sZ>52 aut.</sZ><sZ>53 aut.</sZ><sZ>54 aut.</sZ><sZ>55 aut.</sZ><sZ>56 aut.</sZ><sZ>57 aut.</sZ><sZ>58 aut.</sZ><sZ>59 aut.</sZ><sZ>60 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Korpela, A V" sort="Korpela, A V" uniqKey="Korpela A" first="A. V." last="Korpela">A. V. Korpela</name><affiliation><inist:fA14 i1="03"><s1>MOA Collaboration</s1><s3>MAC</s3><sZ>2 aut.</sZ><sZ>49 aut.</sZ><sZ>50 aut.</sZ><sZ>51 aut.</sZ><sZ>52 aut.</sZ><sZ>53 aut.</sZ><sZ>54 aut.</sZ><sZ>55 aut.</sZ><sZ>56 aut.</sZ><sZ>57 aut.</sZ><sZ>58 aut.</sZ><sZ>59 aut.</sZ><sZ>60 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Masuda, K" sort="Masuda, K" uniqKey="Masuda K" first="K." last="Masuda">K. Masuda</name><affiliation><inist:fA14 i1="03"><s1>MOA Collaboration</s1><s3>MAC</s3><sZ>2 aut.</sZ><sZ>49 aut.</sZ><sZ>50 aut.</sZ><sZ>51 aut.</sZ><sZ>52 aut.</sZ><sZ>53 aut.</sZ><sZ>54 aut.</sZ><sZ>55 aut.</sZ><sZ>56 aut.</sZ><sZ>57 aut.</sZ><sZ>58 aut.</sZ><sZ>59 aut.</sZ><sZ>60 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Matsubara, Y" sort="Matsubara, Y" uniqKey="Matsubara Y" first="Y." last="Matsubara">Y. Matsubara</name><affiliation><inist:fA14 i1="03"><s1>MOA Collaboration</s1><s3>MAC</s3><sZ>2 aut.</sZ><sZ>49 aut.</sZ><sZ>50 aut.</sZ><sZ>51 aut.</sZ><sZ>52 aut.</sZ><sZ>53 aut.</sZ><sZ>54 aut.</sZ><sZ>55 aut.</sZ><sZ>56 aut.</sZ><sZ>57 aut.</sZ><sZ>58 aut.</sZ><sZ>59 aut.</sZ><sZ>60 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Motomura, M" sort="Motomura, M" uniqKey="Motomura M" first="M." last="Motomura">M. Motomura</name><affiliation><inist:fA14 i1="03"><s1>MOA Collaboration</s1><s3>MAC</s3><sZ>2 aut.</sZ><sZ>49 aut.</sZ><sZ>50 aut.</sZ><sZ>51 aut.</sZ><sZ>52 aut.</sZ><sZ>53 aut.</sZ><sZ>54 aut.</sZ><sZ>55 aut.</sZ><sZ>56 aut.</sZ><sZ>57 aut.</sZ><sZ>58 aut.</sZ><sZ>59 aut.</sZ><sZ>60 aut.</sZ></inist:fA14></affiliation></author></analytic><series><title level="j" type="main">Nature : (London)</title><title level="j" type="abbreviated">Nature : (Lond.)</title><idno type="ISSN">0028-0836</idno><imprint><date when="2006">2006</date></imprint></series></biblStruct></sourceDesc><seriesStmt><title level="j" type="main">Nature : (London)</title><title level="j" type="abbreviated">Nature : (Lond.)</title><idno type="ISSN">0028-0836</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Accretion</term><term>Dwarf stars</term><term>Extrasolar planets</term><term>Giant planet</term><term>Gravitational lenses</term><term>M stars</term><term>Microlenses</term><term>Models</term><term>Orbits</term><term>Planet core</term><term>Planetary cosmogony</term><term>Planetesimals</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Microlentille</term><term>Accrétion</term><term>Modèle</term><term>Cosmogonie planétaire</term><term>Planétésimales</term><term>Noyau planétaire</term><term>Etoile M</term><term>Etoile naine</term><term>Planète géante</term><term>Orbite</term><term>Planète extrasolaire</term><term>Lentille gravitationnelle</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">In the favoured core-accretion model of formation of planetary systems, solid planetesimals accumulate to build up planetary cores, which then accrete nebular gas if they are sufficiently massive. Around M-dwarf stars (the most common stars in our Galaxy), this model favours the formation of Earth-mass (M<sub>◦+</sub>) to Neptune-mass planets with orbital radii of 1 to 10 astronomical units (AU), which is consistent with the small number of gas giant planets known to orbit M-dwarf host stars<sup>1-4</sup>. More than 170 extrasolar planets have been discovered with a wide range of masses and orbital periods, but planets of Neptune's mass or less have not hitherto been detected at separations of more than 0.15 AU from normal stars. Here we report the discovery of a 5.5<sup>+5.5</sup><sub>-2.7</sub>M<sub>◦+</sub> planetary companion at a separation of 2.6<sup>+1.5</sup><sub>-0.6</sub>AU from a 0.22<sup>+0.21</sup><sub>-0.11</sub> M<sub>◦.</sub> M-dwarf star, where M<sub>◦.</sub> refers to a solar mass. (We propose to name it OGLE-2005-BLG-390Lb, indicating a planetary mass companion to the lens star of the microlensing event.) The mass is lower than that of GJ876d (ref. 5), although the error bars overlap. Our detection suggests that such cool, sub-Neptune-mass planets may be more common than gas giant planets, as predicted by the core accretion theory.</div></front></TEI><inist><standard h6="B"><pA><fA01 i1="01" i2="1"><s0>0028-0836</s0></fA01><fA02 i1="01"><s0>NATUAS</s0></fA02><fA03 i2="1"><s0>Nature : (Lond.)</s0></fA03><fA05><s2>439</s2></fA05><fA06><s2>7075</s2></fA06><fA08 i1="01" i2="1" l="ENG"><s1>Discovery of a cool planet of 5.5 earth masses through gravitational microlensing</s1></fA08><fA11 i1="01" i2="1"><s1>BEAULIEU (J.-P.)</s1></fA11><fA11 i1="02" i2="1"><s1>BENNETT (D. P.)</s1></fA11><fA11 i1="03" i2="1"><s1>FOUQUE (P.)</s1></fA11><fA11 i1="04" i2="1"><s1>WILLIAMS (A.)</s1></fA11><fA11 i1="05" i2="1"><s1>DOMINIK (M.)</s1></fA11><fA11 i1="06" i2="1"><s1>JØRGENSEN (U. G.)</s1></fA11><fA11 i1="07" i2="1"><s1>KUBAS (D.)</s1></fA11><fA11 i1="08" i2="1"><s1>CASSAN (A.)</s1></fA11><fA11 i1="09" i2="1"><s1>COUTURES (C.)</s1></fA11><fA11 i1="10" i2="1"><s1>GREENHILL (J.)</s1></fA11><fA11 i1="11" i2="1"><s1>HILL (K.)</s1></fA11><fA11 i1="12" i2="1"><s1>MENZIES (J.)</s1></fA11><fA11 i1="13" i2="1"><s1>SACKETT (P. D.)</s1></fA11><fA11 i1="14" i2="1"><s1>ALBROW (M.)</s1></fA11><fA11 i1="15" i2="1"><s1>BRILLANT (S.)</s1></fA11><fA11 i1="16" i2="1"><s1>CALDWELL (J. A. R.)</s1></fA11><fA11 i1="17" i2="1"><s1>CALITZ (J. J.)</s1></fA11><fA11 i1="18" i2="1"><s1>COOK (K. H.)</s1></fA11><fA11 i1="19" i2="1"><s1>CORRALES (E.)</s1></fA11><fA11 i1="20" i2="1"><s1>DESORT (M.)</s1></fA11><fA11 i1="21" i2="1"><s1>DIETERS (S.)</s1></fA11><fA11 i1="22" i2="1"><s1>DOMINIS (D.)</s1></fA11><fA11 i1="23" i2="1"><s1>DONATOWICZ (J.)</s1></fA11><fA11 i1="24" i2="1"><s1>HOFFMAN (M.)</s1></fA11><fA11 i1="25" i2="1"><s1>KANE (S.)</s1></fA11><fA11 i1="26" i2="1"><s1>MARQUETTE (J.-B.)</s1></fA11><fA11 i1="27" i2="1"><s1>MARTIN (R.)</s1></fA11><fA11 i1="28" i2="1"><s1>MEINTJES (P.)</s1></fA11><fA11 i1="29" i2="1"><s1>POLLARD (K.)</s1></fA11><fA11 i1="30" i2="1"><s1>SAHU (K.)</s1></fA11><fA11 i1="31" i2="1"><s1>VINTER (C.)</s1></fA11><fA11 i1="32" i2="1"><s1>WAMBSGANSS (J.)</s1></fA11><fA11 i1="33" i2="1"><s1>WOLLER (K.)</s1></fA11><fA11 i1="34" i2="1"><s1>HORNE (K.)</s1></fA11><fA11 i1="35" i2="1"><s1>STEELE (I.)</s1></fA11><fA11 i1="36" i2="1"><s1>BRAMICH (D. M.)</s1></fA11><fA11 i1="37" i2="1"><s1>BURGDORF (M.)</s1></fA11><fA11 i1="38" i2="1"><s1>SNODGRASS (C.)</s1></fA11><fA11 i1="39" i2="1"><s1>BODE (M.)</s1></fA11><fA11 i1="40" i2="1"><s1>UDALSKI (A.)</s1></fA11><fA11 i1="41" i2="1"><s1>SZYMANSKI (M. K.)</s1></fA11><fA11 i1="42" i2="1"><s1>KUBIAK (M.)</s1></fA11><fA11 i1="43" i2="1"><s1>WIECKOWSKI (T.)</s1></fA11><fA11 i1="44" i2="1"><s1>PIETRZYNSKI (G.)</s1></fA11><fA11 i1="45" i2="1"><s1>SOSZYNSKI (I.)</s1></fA11><fA11 i1="46" i2="1"><s1>SZEWCZYK (O.)</s1></fA11><fA11 i1="47" i2="1"><s1>WYRZYKOWSKI (T.)</s1></fA11><fA11 i1="48" i2="1"><s1>PACZYNSKI (B.)</s1></fA11><fA11 i1="49" i2="1"><s1>ABE (F.)</s1></fA11><fA11 i1="50" i2="1"><s1>BOND (I. A.)</s1></fA11><fA11 i1="51" i2="1"><s1>BRITTON (T. R.)</s1></fA11><fA11 i1="52" i2="1"><s1>GILMORE (A. C.)</s1></fA11><fA11 i1="53" i2="1"><s1>HEARNSHAW (J. B.)</s1></fA11><fA11 i1="54" i2="1"><s1>ITOW (Y.)</s1></fA11><fA11 i1="55" i2="1"><s1>KAMIYA (K.)</s1></fA11><fA11 i1="56" i2="1"><s1>KILMARTIN (P. M.)</s1></fA11><fA11 i1="57" i2="1"><s1>KORPELA (A. V.)</s1></fA11><fA11 i1="58" i2="1"><s1>MASUDA (K.)</s1></fA11><fA11 i1="59" i2="1"><s1>MATSUBARA (Y.)</s1></fA11><fA11 i1="60" i2="1"><s1>MOTOMURA (M.)</s1></fA11><fA14 i1="01"><s1>PLANET/RoboNet Collaboration</s1><s3>FRA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>9 aut.</sZ><sZ>10 aut.</sZ><sZ>11 aut.</sZ><sZ>12 aut.</sZ><sZ>13 aut.</sZ><sZ>14 aut.</sZ><sZ>15 aut.</sZ><sZ>16 aut.</sZ><sZ>17 aut.</sZ><sZ>18 aut.</sZ><sZ>19 aut.</sZ><sZ>20 aut.</sZ></fA14><fA14 i1="02"><s1>Institut d'Astrophysique de Paris, CNRS, Université Pierre et Marie Curie UMR7095, 98bis Boulevard Arago</s1><s2>75014 Pans</s2><s3>FRA</s3><sZ>1 aut.</sZ><sZ>8 aut.</sZ><sZ>19 aut.</sZ><sZ>20 aut.</sZ><sZ>26 aut.</sZ></fA14><fA14 i1="03"><s1>MOA Collaboration</s1><s3>MAC</s3><sZ>2 aut.</sZ><sZ>49 aut.</sZ><sZ>50 aut.</sZ><sZ>51 aut.</sZ><sZ>52 aut.</sZ><sZ>53 aut.</sZ><sZ>54 aut.</sZ><sZ>55 aut.</sZ><sZ>56 aut.</sZ><sZ>57 aut.</sZ><sZ>58 aut.</sZ><sZ>59 aut.</sZ><sZ>60 aut.</sZ></fA14><fA14 i1="04"><s1>University of Notre Dame, Department of Physics</s1><s2>Notre Dame, Indiana 46556-5670</s2><s3>USA</s3><sZ>2 aut.</sZ></fA14><fA14 i1="05"><s1>Observatoire Midi-Pyrénées, Laboratoire d'Astrophysique, UMR 5572, Université Paul Sabatier-Toulouse 3,14 avenue Edouard Belin</s1><s2>31400 Toulouse</s2><s3>FRA</s3><sZ>3 aut.</sZ></fA14><fA14 i1="06"><s1>Perth Observatory, Walnut Road</s1><s2>Bickley, Perth, WA 6076</s2><s3>AUS</s3><sZ>4 aut.</sZ><sZ>27 aut.</sZ></fA14><fA14 i1="07"><s1>Scottish Universities Physics Alliance, University of St Andrews, School of Physics and Astronomy</s1><s2>North Haugh, St Andrews KY16 9SS</s2><s3>GBR</s3><sZ>5 aut.</sZ><sZ>34 aut.</sZ><sZ>36 aut.</sZ></fA14><fA14 i1="08"><s1>Niels Bohr Institutet, Astronomisk Observatorium, Juliane Manes Vej 30</s1><s2>2100 København</s2><s3>DNK</s3><sZ>6 aut.</sZ><sZ>31 aut.</sZ><sZ>33 aut.</sZ></fA14><fA14 i1="09"><s1>European Southern Observatory</s1><s2>Casilla 19001, Santiago 19</s2><s3>CHL</s3><sZ>7 aut.</sZ><sZ>15 aut.</sZ></fA14><fA14 i1="10"><s1>CEA DAPNIA/SPP Saclay</s1><s2>91191 Gif-sur-Yvette</s2><s3>FRA</s3><sZ>9 aut.</sZ></fA14><fA20><s1>437-440</s1></fA20><fA21><s1>2006</s1></fA21><fA23 i1="01"><s0>ENG</s0></fA23><fA43 i1="01"><s1>INIST</s1><s2>142</s2><s5>354000134741690160</s5></fA43><fA44><s0>0000</s0><s1>© 2006 INIST-CNRS. All rights reserved.</s1></fA44><fA45><s0>30 ref.</s0></fA45><fA47 i1="01" i2="1"><s0>06-0192157</s0></fA47><fA60><s1>P</s1></fA60><fA61><s0>A</s0></fA61><fA64 i1="01" i2="1"><s0>Nature : (London)</s0></fA64><fA66 i1="01"><s0>GBR</s0></fA66><fC01 i1="01" l="ENG"><s0>In the favoured core-accretion model of formation of planetary systems, solid planetesimals accumulate to build up planetary cores, which then accrete nebular gas if they are sufficiently massive. Around M-dwarf stars (the most common stars in our Galaxy), this model favours the formation of Earth-mass (M<sub>◦+</sub>) to Neptune-mass planets with orbital radii of 1 to 10 astronomical units (AU), which is consistent with the small number of gas giant planets known to orbit M-dwarf host stars<sup>1-4</sup>. More than 170 extrasolar planets have been discovered with a wide range of masses and orbital periods, but planets of Neptune's mass or less have not hitherto been detected at separations of more than 0.15 AU from normal stars. Here we report the discovery of a 5.5<sup>+5.5</sup><sub>-2.7</sub>M<sub>◦+</sub> planetary companion at a separation of 2.6<sup>+1.5</sup><sub>-0.6</sub>AU from a 0.22<sup>+0.21</sup><sub>-0.11</sub> M<sub>◦.</sub> M-dwarf star, where M<sub>◦.</sub> refers to a solar mass. (We propose to name it OGLE-2005-BLG-390Lb, indicating a planetary mass companion to the lens star of the microlensing event.) The mass is lower than that of GJ876d (ref. 5), although the error bars overlap. Our detection suggests that such cool, sub-Neptune-mass planets may be more common than gas giant planets, as predicted by the core accretion theory.</s0></fC01><fC02 i1="01" i2="3"><s0>001E03C82C</s0></fC02><fC03 i1="01" i2="3" l="FRE"><s0>Microlentille</s0><s5>27</s5></fC03><fC03 i1="01" i2="3" l="ENG"><s0>Microlenses</s0><s5>27</s5></fC03><fC03 i1="02" i2="3" l="FRE"><s0>Accrétion</s0><s5>28</s5></fC03><fC03 i1="02" i2="3" l="ENG"><s0>Accretion</s0><s5>28</s5></fC03><fC03 i1="03" i2="X" l="FRE"><s0>Modèle</s0><s5>29</s5></fC03><fC03 i1="03" i2="X" l="ENG"><s0>Models</s0><s5>29</s5></fC03><fC03 i1="03" i2="X" l="SPA"><s0>Modelo</s0><s5>29</s5></fC03><fC03 i1="04" i2="X" l="FRE"><s0>Cosmogonie planétaire</s0><s5>30</s5></fC03><fC03 i1="04" i2="X" l="ENG"><s0>Planetary cosmogony</s0><s5>30</s5></fC03><fC03 i1="04" i2="X" l="SPA"><s0>Cosmogonía planetaria</s0><s5>30</s5></fC03><fC03 i1="05" i2="3" l="FRE"><s0>Planétésimales</s0><s5>31</s5></fC03><fC03 i1="05" i2="3" l="ENG"><s0>Planetesimals</s0><s5>31</s5></fC03><fC03 i1="06" i2="X" l="FRE"><s0>Noyau planétaire</s0><s5>32</s5></fC03><fC03 i1="06" i2="X" l="ENG"><s0>Planet core</s0><s5>32</s5></fC03><fC03 i1="06" i2="X" l="SPA"><s0>Núcleo planetario</s0><s5>32</s5></fC03><fC03 i1="07" i2="3" l="FRE"><s0>Etoile M</s0><s5>33</s5></fC03><fC03 i1="07" i2="3" l="ENG"><s0>M stars</s0><s5>33</s5></fC03><fC03 i1="08" i2="3" l="FRE"><s0>Etoile naine</s0><s5>34</s5></fC03><fC03 i1="08" i2="3" l="ENG"><s0>Dwarf stars</s0><s5>34</s5></fC03><fC03 i1="09" i2="X" l="FRE"><s0>Planète géante</s0><s5>36</s5></fC03><fC03 i1="09" i2="X" l="ENG"><s0>Giant planet</s0><s5>36</s5></fC03><fC03 i1="09" i2="X" l="SPA"><s0>Planeta gigante</s0><s5>36</s5></fC03><fC03 i1="10" i2="3" l="FRE"><s0>Orbite</s0><s5>37</s5></fC03><fC03 i1="10" i2="3" l="ENG"><s0>Orbits</s0><s5>37</s5></fC03><fC03 i1="11" i2="3" l="FRE"><s0>Planète extrasolaire</s0><s5>38</s5></fC03><fC03 i1="11" i2="3" l="ENG"><s0>Extrasolar planets</s0><s5>38</s5></fC03><fC03 i1="12" i2="3" l="FRE"><s0>Lentille gravitationnelle</s0><s5>39</s5></fC03><fC03 i1="12" i2="3" l="ENG"><s0>Gravitational lenses</s0><s5>39</s5></fC03><fN21><s1>114</s1></fN21></pA></standard><server><NO>PASCAL 06-0192157 INIST</NO><ET>Discovery of a cool planet of 5.5 earth masses through gravitational microlensing</ET><AU>BEAULIEU (J.-P.); BENNETT (D. P.); FOUQUE (P.); WILLIAMS (A.); DOMINIK (M.); JØRGENSEN (U. G.); KUBAS (D.); CASSAN (A.); COUTURES (C.); GREENHILL (J.); HILL (K.); MENZIES (J.); SACKETT (P. D.); ALBROW (M.); BRILLANT (S.); CALDWELL (J. A. R.); CALITZ (J. J.); COOK (K. H.); CORRALES (E.); DESORT (M.); DIETERS (S.); DOMINIS (D.); DONATOWICZ (J.); HOFFMAN (M.); KANE (S.); MARQUETTE (J.-B.); MARTIN (R.); MEINTJES (P.); POLLARD (K.); SAHU (K.); VINTER (C.); WAMBSGANSS (J.); WOLLER (K.); HORNE (K.); STEELE (I.); BRAMICH (D. M.); BURGDORF (M.); SNODGRASS (C.); BODE (M.); UDALSKI (A.); SZYMANSKI (M. K.); KUBIAK (M.); WIECKOWSKI (T.); PIETRZYNSKI (G.); SOSZYNSKI (I.); SZEWCZYK (O.); WYRZYKOWSKI (T.); PACZYNSKI (B.); ABE (F.); BOND (I. A.); BRITTON (T. R.); GILMORE (A. C.); HEARNSHAW (J. B.); ITOW (Y.); KAMIYA (K.); KILMARTIN (P. M.); KORPELA (A. V.); MASUDA (K.); MATSUBARA (Y.); MOTOMURA (M.)</AU><AF>PLANET/RoboNet Collaboration/France (1 aut., 2 aut., 3 aut., 4 aut., 5 aut., 6 aut., 7 aut., 8 aut., 9 aut., 10 aut., 11 aut., 12 aut., 13 aut., 14 aut., 15 aut., 16 aut., 17 aut., 18 aut., 19 aut., 20 aut.); Institut d'Astrophysique de Paris, CNRS, Université Pierre et Marie Curie UMR7095, 98bis Boulevard Arago/75014 Pans/France (1 aut., 8 aut., 19 aut., 20 aut., 26 aut.); MOA Collaboration/Macao (2 aut., 49 aut., 50 aut., 51 aut., 52 aut., 53 aut., 54 aut., 55 aut., 56 aut., 57 aut., 58 aut., 59 aut., 60 aut.); University of Notre Dame, Department of Physics/Notre Dame, Indiana 46556-5670/Etats-Unis (2 aut.); Observatoire Midi-Pyrénées, Laboratoire d'Astrophysique, UMR 5572, Université Paul Sabatier-Toulouse 3,14 avenue Edouard Belin/31400 Toulouse/France (3 aut.); Perth Observatory, Walnut Road/Bickley, Perth, WA 6076/Australie (4 aut., 27 aut.); Scottish Universities Physics Alliance, University of St Andrews, School of Physics and Astronomy/North Haugh, St Andrews KY16 9SS/Royaume-Uni (5 aut., 34 aut., 36 aut.); Niels Bohr Institutet, Astronomisk Observatorium, Juliane Manes Vej 30/2100 København/Danemark (6 aut., 31 aut., 33 aut.); European Southern Observatory/Casilla 19001, Santiago 19/Chili (7 aut., 15 aut.); CEA DAPNIA/SPP Saclay/91191 Gif-sur-Yvette/France (9 aut.)</AF><DT>Publication en série; Niveau analytique</DT><SO>Nature : (London); ISSN 0028-0836; Coden NATUAS; Royaume-Uni; Da. 2006; Vol. 439; No. 7075; Pp. 437-440; Bibl. 30 ref.</SO><LA>Anglais</LA><EA>In the favoured core-accretion model of formation of planetary systems, solid planetesimals accumulate to build up planetary cores, which then accrete nebular gas if they are sufficiently massive. Around M-dwarf stars (the most common stars in our Galaxy), this model favours the formation of Earth-mass (M<sub>◦+</sub>) to Neptune-mass planets with orbital radii of 1 to 10 astronomical units (AU), which is consistent with the small number of gas giant planets known to orbit M-dwarf host stars<sup>1-4</sup>. More than 170 extrasolar planets have been discovered with a wide range of masses and orbital periods, but planets of Neptune's mass or less have not hitherto been detected at separations of more than 0.15 AU from normal stars. Here we report the discovery of a 5.5<sup>+5.5</sup><sub>-2.7</sub>M<sub>◦+</sub> planetary companion at a separation of 2.6<sup>+1.5</sup><sub>-0.6</sub>AU from a 0.22<sup>+0.21</sup><sub>-0.11</sub> M<sub>◦.</sub> M-dwarf star, where M<sub>◦.</sub> refers to a solar mass. (We propose to name it OGLE-2005-BLG-390Lb, indicating a planetary mass companion to the lens star of the microlensing event.) The mass is lower than that of GJ876d (ref. 5), although the error bars overlap. Our detection suggests that such cool, sub-Neptune-mass planets may be more common than gas giant planets, as predicted by the core accretion theory.</EA><CC>001E03C82C</CC><FD>Microlentille; Accrétion; Modèle; Cosmogonie planétaire; Planétésimales; Noyau planétaire; Etoile M; Etoile naine; Planète géante; Orbite; Planète extrasolaire; Lentille gravitationnelle</FD><ED>Microlenses; Accretion; Models; Planetary cosmogony; Planetesimals; Planet core; M stars; Dwarf stars; Giant planet; Orbits; Extrasolar planets; Gravitational lenses</ED><SD>Modelo; Cosmogonía planetaria; Núcleo planetario; Planeta gigante</SD><LO>INIST-142.354000134741690160</LO><ID>06-0192157</ID></server></inist></record>Pour manipuler ce document sous Unix (Dilib)
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