Search

5 Jul 2018: N(H I) = 2.5 1020 cm2. Fe/H = 1/200 solar. Very Metal Poor DLAs are the choice astrophysical environments for measuring the primordial abundance of deuterium.

30 Jul 2018: MNRAS 000, 1–23 (2015) Preprint 30 July 2018 Compiled using MNRAS LATEX style file v3.0. Using warm dust to constrain unseen planets. Amy Bonsor1, Mark C. Wyatt1, Quentin Kral1, Grant Kennedy2,3, Andrew. Shannon4,5 and Steve Ertel61Institute of

31 Jul 2018: Approximately 85 planets could be habitable (radii between 0.5 Rand 1.75 R and equilibrium temperatures between 200 K and 450 K) andwould be prime targets for follow-up spectroscopic ... Earth orbiting α Cen and 10 small planets (1 to 4 R) with

2 Apr 2018: arX. iv:1. 803. 1126. 5v1. [as. tro-. ph.S. R]. 29. Mar. 201. 8Draft version April 2, 2018. Typeset using LATEX twocolumn style in AASTeX61. THE HOSTS SURVEY – EXOZODIACAL DUST MEASUREMENTS FOR 30 STARS. Ertel, S.,1 Defrère, D.,2 Hinz, P.,1

30 Jul 2018: 2002). [20] Mérand, A., Bordé, P., and Coudé du Foresto, V., “A catalog of bright calibrator stars for 200-m baselinenear-infrared stellar interferometry,” A&A 433, 1155–1162 (Apr.

23 Aug 2018: MNRAS 000, 1–13 (2018) Preprint 23 August 2018 Compiled using MNRAS LATEX style file v3.0. Fast spectrophotometry of WD 1145017. Paula Izquierdo1,2?, Pablo Rodŕıguez-Gil1,2, Boris T. Gänsicke3,4, Alexander J. Mustill5,Odette Toloza3,

9 Nov 2018: In total the datacomprise four years of photometry for roughly 200,000 dis-tinct stars.

22 Nov 2018: 10 correspond tothe locations and radial velocities at which gas is expectedto emit if on a circular orbit at 40 and 200 au (assuming a1.77 M star, Moór et al. ... 2015). The PV-diagram thus tellsus that the bulk of the gas disc is between 40 and 200

30 Jul 2018: MNRAS 479, 2649–2672 (2018) doi:10.1093/mnras/sty1677Advance Access publication 2018 June 26. Cometary impactors on the TRAPPIST-1 planets can destroy all planetaryatmospheres and rebuild secondary atmospheres on planets f, g, and h. Quentin

31 Jul 2018: 4.1 Planet mass and semi-major axis distribution. We consider a chain of planets on circular co-planar orbits,with masses varying from 1 to 200 M (0.63 MJup) ... Inorder to minimise random effects caused by the finite num-ber of particles used in these