http://chineseinput.net/에서 pinyin(병음)방식으로 중국어를 변환할 수 있습니다.
변환된 중국어를 복사하여 사용하시면 됩니다.
SOME REMARKS ON M-IDEALS AND STRONG PROXIMINALITY
Finet, Chaterine,Quarta, Lucas Korean Mathematical Society 2003 대한수학회보 Vol.40 No.3
We prove that every M-ideal is strongly proximinal and that, for any Banach space X, $K(X,\;c_0)$ is an M-ideal in $L(X,\;\ell^{\infty})$.
Some remarks on $M$-ideals and strong proximinality
Catherine Finet,Lucas Quarta 대한수학회 2003 대한수학회보 Vol.40 No.3
We prove that every M-ideal is strongly proximinal and that, forany Banach space X, K(X,c_0) is an M-ideal inL(X,ell^infty).
Flux and color variations of the doubly imaged quasar UM673
Ricci, D.,Elyiv, A.,Finet, F.,Wertz, O.,Alsubai, K.,Anguita, T.,Bozza, V.,Browne, P.,Burgdorf, M.,Calchi Novati, S.,Dodds, P.,Dominik, M.,Dreizler, S.,Gerner, T.,Glitrup, M.,Grundahl, F.,Hardis, S.,Ha EDP Sciences 2013 Astronomy and astrophysics Vol.551 No.-
Transits and starspots in the WASP-6 planetary system
Tregloan-Reed, J.,Southworth, J.,Burgdorf, M.,Novati, S. C.,Dominik, M.,Finet, F.,Jorgensen, U. G.,Maier, G.,Mancini, L.,Prof, S.,Ricci, D.,Snodgrass, C.,Bozza, V.,Browne, P.,Dodds, P.,Gerner, T.,Harp Oxford University Press 2015 Monthly notices of the Royal Astronomical Society Vol.450 No.2
A SUB-SATURN MASS PLANET, MOA-2009-BLG-319Lb
Miyake, N.,Sumi, T.,Dong, Subo,Street, R.,Mancini, L.,Gould, A.,Bennett, D. P.,Tsapras, Y.,Yee, J. C.,Albrow, M. D.,Bond, I. A.,Fouqué,, P.,Browne, P.,Han, C.,Snodgrass, C.,Finet, F.,Furusawa, K IOP Publishing 2011 The Astrophysical journal Vol.728 No.2
<P>We report the gravitational microlensing discovery of a sub-Saturn mass planet, MOA-2009-BLG-319Lb, orbiting a K-or M-dwarf star in the inner Galactic disk or Galactic bulge. The high-cadence observations of the MOA-II survey discovered this microlensing event and enabled its identification as a high-magnification event approximately 24 hr prior to peak magnification. As a result, the planetary signal at the peak of this light curve was observed by 20 different telescopes, which is the largest number of telescopes to contribute to a planetary discovery to date. The microlensing model for this event indicates a planet-star mass ratio of q = (3.95 +/- 0.02) x 10(-4) and a separation of d = 0.97537 +/- 0.00007 in units of the Einstein radius. A Bayesian analysis based on the measured Einstein radius crossing time, t(E), and angular Einstein radius,theta(E), along with a standard Galactic model indicates a host star mass of M-L = 0.38(-0.18)(+0.34) M-circle dot and a planet mass of M-p = 50(-24)(+44)M(circle plus), which is half the mass of Saturn. This analysis also yields a planet-star three-dimensional separation of a = 2.4(-0.6)(+1.2) AU and a distance to the planetary system of D-L = 6.1(-1.2)(+1.1) kpc. This separation is similar to 2 times the distance of the snow line, a separation similar to most of the other planets discovered by microlensing.</P>