Search

18 Sep 2007: assumingF /F p 0.1disk a limit of , based on Su et al. ... 3. Stellar multiplicity.—With 50% of target stars havinganother star as a companion.

7 Jul 2012: Previous effortsfor theHerschel (Pilbratt et al. 2010) Disc Emission via a Bias-free. ... A total of 144655sources have a WISE detection in at least one band.

19 Feb 2010: Weshow that there is no significant statistical difference between fractional excessesof A-stars. ... 5). We also assume that the central star acts like a black-body.

21 Jan 2014: a useful evolutionary sequence it is important to interpret in-dividual objects carefully. ... 4.8. Schneider et al. (2013)report a detection in the XMM-Newton Serendipitous Source Cat-alog (Watson et al.

6 Apr 2010: possibilitiesinclude dynamical scattering by a migrating planet, see e.g.Gomes et al. ... This source together with HD 31295 andHD 38206 are described in Appendix A.

25 Oct 2009: by postulating a populationof parent planetesimals on highly eccentric orbits (e 0.3). ... Rcc(Dmax) = KMtotv8/3k (a)a. 3(4πImax)1S(e), (16). S2d(e) =X. r̄. r̄2dr̄1σ̄(r̄)2〈[vrel/vk(a)]8/3〉(r̄), (17).

5 Jul 2011: Four 3’ scan legs wereperformed per map with a 2” separation between legs. ... 2008) and to a theoretical PSF (gen-. 2010 RAS, MNRAS 000, 1–20.

5 Oct 2007: within a massive comet or asteroid (processed, differentiated planetesimals) belt, (iv) recent col-. ... performed (Watson et al. 2004). The reduction and analysis of the spectra was conducted with.

23 Nov 2021: These instru-ments reveal a wealth of substructures within disks, forboth targeted (e.g. ... We assumehere a gas-to-dust mass ratio of 100 and indicate the.

18 Aug 2020: We start with a simple estimate. Assuming the PPDmass to be 0.1M? ... A-stars with2 solar masses) can be higher by a factor 2.7.

29 Apr 2008: 2005), thoughtto be there because this is a young (12Myr, Zuckerman et al. ... We con-sider a detection to be whereS op > 3. 4.1.1.

10 Feb 2021: 2017), a possibility also not ruled out by far-IRsurveys of star forming regions. ... Withinthe inner 0.68′′ radius circle there is a 2.8𝜎 significant detection.

28 Oct 2013: Kervella P., Thévenin F., Di Folco E., Ségransan D., 2004,A&A 426, 297. ... von Braun K. et al., 2011, ApJ 729, L26. Watson C.A.

17 Dec 2014: mass component of a protoplanetary disk, is no longer. present in debris disks. ... this denomination. A catalogue summarising this class. is given in Thé et al.

11 Apr 2019: A typical valuefor λmax within our galaxy is 550 nm (Serkowski et al. ... 2010). is the Sun at its centre, a fact which naturally explains thephenomenon.

22 Aug 2014: Infra-red excess detections are generally well approxi-mated by a single blackbody. ... For example,ζ Lep shows evidence for extra emissionabove a blackbody around 10µm (Fig.

29 Apr 2016: arX. iv:1. 604. 0828. 6v1. [ast. ro-p. h.E. P]. 28 A. ... by high orbital eccentricity comets,is likewise difficult to achieve from a dynamical perspective.

2 Nov 2015: M. Ansdell1,10, E. Gaidos2,3,4,10, S. A. Rappaport5, T. L. Jacobs6, D. ... M. LaCourse6, K. J. Jek6, A. W. Mann7,10, M.C. Wyatt8, G.

8 Jan 2019: a sharp outer edge, similar to the morphology seen byHST (Golimowski et al. ... 2. One way of describingthis is to define Σr(a) = n(a)/(2πa), where a = a(r, φ) andΣr(a) is the surface density that would have resulted fromthe given

23 Dec 2017: WATSON,130 R.C. WEIR,4. KLAUS WENZEL,131 MICHAEL W. WILLIAMSON,56 JASON T. WRIGHT,10, 11, 132 M. ... TheLCOGT observations are a product of a successful crowd-funding effort through Kickstarter3.