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13 Mar 2012: 3/12/12 Astroparticle 24. Exploit fact that gravity couples to all particle types! ... Assume system created in disk - get minimum lifetime for black hole, 24 Myr, and hence max curvature of ADS bulk - 80 microns!

27 Apr 2012: 8. VST update -------------- As noted earlier, since February 29th Internet transfers of VST data from Paranal - Garching have been using the EVALSO link and VST data is now available 24 hours

5 Dec 2012: The one in question is at http://www.eso.org/sci/facilities/paranal/instruments/vircam/news.html and shows it was 2010-04-24/2010-05-06.

24 Aug 2012: transfer over the Internet some 24 hours later.

5 Dec 2012: wrong end time and date for an OB. An example of the latter is below 2012-08-24 VIS 179.A-2010(F) 812323 0.00 A

27 Feb 2012: 2/20/12 Astroparticle 24.  Bulk region.  Co-annihilation region.  Focus point region.

12 Mar 2012: Apply local SU(5) gauge symmetry - get 24 gauge bosons: γ, W+, W-, Z, 8 gluons and 12 X,Y bosons mediating quark-lepton transitions!These violate baryon and lepton number! ... and sgn(µ) as in SUGRA!Cgrav! Coupling for decays into gravitinos! 3/2/12

10 Dec 2012: There isboth cool dust (observable to Herschel) and warm dust(evident from IRS and MIPS 24 excesses). ... In the context of the wide belt imaging model, the IRSand MIPS 24 excesses are attributed to a warm innerring.

29 Jun 2012: However, progress will be difficult.Table 3 inJewitt & Haghighipour(2007) shows that the faintestknown irregulars at Saturn have R magnitudes of 24.5,3 and thedeepest survey for Uranian irregulars had ... 3 The faintest published survey hasR = 24.5

19 Jun 2012: Byconsidering the luminosity of dust produced in collisions within the boulder-debris distributionwe find that the Moon-forming impact would have been readily detectable around other stars inSpitzer 24 µm surveys

5 Oct 2012: β Uma PACS 70/160 1342220802/3 2011-04-29. PACS 100/160 1342197015/6 2010-05-24. SPIRE 1342195687 2010-04-29. ... PSF fit500 4.24.9 0.420.01 3.84.9 PSF fit.

7 Nov 2012: 24.8 2,14.8 1 arcsec, 75 4.5 at 160 μm. ... Photometry on the 24 μm image was used in the spectral energydistribution (SED) modelling.

23 Oct 2012: which could be readily detectable around other stars by Spitzer 24 μm surveys for 25 Myr after. ... SiO h (24). which occurs with a rate coefficient m3 s-1 (Andreazza et al.

24 Nov 2012: Finally, we used the SPIRE 3σ upper limits as a constraint toreject any model with a flux density of the dust emission largerthan 24 mJy at 250µm. ... The upper inset zooms on the IRS wavelengths and displays spectra asSν(λ/24)2 on a linear scale

22 May 2012: However, the lowest mass planets scatter test particles moreweakly and thus fewer test particles end up with e > eSD = 0.24,our definition of the scattered disc and MSD is low

7 Jul 2012: Also shown is the sensitivity with MIPS at 24 and 70µm to55 Cancri, a typical nearby star at 12pc withKs 4.2 (grey lines).

30 Oct 2012: 2009), with q 24 au and a 796 au, and 2000 OO67 (Veillet, Doressoundiram &. Marsden 2001; Millis et al. 2002), with q 21 au and a 552 au.The perihelia and

24 Jan 2012: CURRICULUM VITAE. FULL NAME: George Petros EFSTATHIOUNATIONALITY: BritishDATE OF BIRTH: 2nd Sept 1955. QUALIFICATIONS. Dates Academic Institution Degree. 10/73 to 7/76 Keble College, Oxford. B.A. in Physics10/76 to 9/79 Department of Physics, Ph.D.

12 Jan 2012: 8 arcminaway to the SE (PA = 120) that is visible at 24, 70, and100µm.

1 Aug 2012: edu. Received 2008 November 24; accepted 2009 June 16; published 2009 August 7. ... This agrees well with the200 K temperature of the large, cool grain dust grains fromthis work, and with Wyatt et al.’s (2007b) Spitzer 24/70 μmbased estimate of 4–5