Vibration and dissociation coupling behind strong shock waves. Paper presented at the Symposium on Dynamics of Manned Lifting Planetary Entry,

Cover title.

A new general catalogue of nebulae and clusters of stars, being the catalogue of the late Sir John F.W. Herschel.

Mode of access: Internet.

Astronomy improved: or, A new theory of the harmonious regularity observable in the mechanism or movements of the planetary system. In three lectures, read in the chapel of Yale-college, in New-Haven. Begun February 17, 1781 ...

Evans 18797.

Celestial scenery ; or, The wonders of the planetary system displayed /

Mode of access: Internet.

Mathematical tracts on the lunar and planetary theories, the figure of the earth, precession and nutation, the calculus of variations, and the undulatory theory of optics. Designed for the use of students in the university.

Mode of access: Internet.

The planetary product in 1975 and a preview for 1976.

Mode of access: Internet.

Celestial scenery; or, The wonders of the planetary system displayed; illustrating the perfections of deity and a plurality of worlds.

Mode of access: Internet.

Celestial scenery; or, The wonders of the planetary system displayed; illustrating the perfections of the deity and a plurality of worlds.

Last leaf of text (p. 407-408) wanting.

Researches on the evolution of the stellar systems ...

v. 1. On the universality of the law of gravitation and on the orbits and general characteristics of binary stars.--v. 2. The capture theory of cosmical evolution, founded on dynamical principles and illustrated by phenomena observed in the spiral nebulae, the planetary system, the double and multiple stars and clusters and the star-clouds of the Milky way.

Dynamics and thermodynamics of planetary entry.

Includes bibliography.

The planetary product /

Mode of access: Internet.

The planetary man.

v.1. A noetic prelude to a united world.

The role of the 8-18 helix of CGRP 8-37 in mediating high affinity binding to CGRP receptors; coulombic and steric interactions

1. The role of individual residues in the 8-18 helix of CGRP 8-37 in promoting high-affinity binding to CGRP 1 receptors expressed on rat L6 and human SK-N-MC cells has been examined. The relative potencies of various derivatives were estimated from their ability to inhibit the human αCGRP-mediated increase in cyclic AMP production and the binding of [ 125I]-human αCGRP. 3. Arg 11 and Arg 18 were replaced by serines to give [Ser 11.18]CGRP 8-37. These bound with pKi values <6 to SK-N-MC cells and had apparent pA 2 values of 5.81 ± 0.04 and 5.31 ± 0.11 on SK-N-MC and L6 cells. CGRP 8-37 had a pKi of 8.22 on SK-N-MC cells and pK b values on the above cell lines of 8.95±0.04 and 8.76±0.04. 3. The arginines were replaced with glutamic acid residues. [Glu 11]CGRP 8-37 had a pK b of 7.14±0.14 on SK-N-MC cells (pKi=7.05±0.05) and 6.99±0.08 on L6 cells. [Glu 18]CGRP 8-37 had a pK b of 7.10±0.0.08 on SK-N-MC cells (pKi=6.91±0.23) and 7.12±0.09 on L6 cells. 4. Leu 12, Leu 15 and Leu 16 were replaced by benzoyl-phenylalanine (bpa) residues. On SK-N-MC cells, the apparent pA 2 values of [bpa 12]-, [bpa 15]- and [bpa 16]CGRP 8-37 were respectively 7.43±0.23, 8.34±0.11 and 5.66±0.16 (pKi values of 7.14±0.17, 7.66±0.21 and <6): on L6 cells they were 7.96±0.36, 8.28±0.21 and 6.09±0.04 (all n=3). 5. It is concluded that the Arg 11 and Arg 18 are involved in specific electrostatic interactions with other residues, either on the CGRP 1 receptors or elsewhere on CGRP 8-37. Leu 16 is in a conformationally restricted site when CGRP 8-37 binds to CGRP 1 receptors, unlike Leu 12 and Leu 15.

The VLT-FLAMES tarantula survey:XII. Rotational velocities of the single O-type stars

Context. The 30 Doradus (30 Dor) region of the Large Magellanic Cloud, also known as the Tarantula nebula, is the nearest starburst region. It contains the richest population of massive stars in the Local Group, and it is thus the best possible laboratory to investigate open questions on the formation and evolution of massive stars. Aims. Using ground-based multi-object optical spectroscopy obtained in the framework of the VLT-FLAMES Tarantula Survey (VFTS), we aim to establish the (projected) rotational velocity distribution for a sample of 216 presumably single O-type stars in 30 Dor. The sample is large enough to obtain statistically significant information and to search for variations among subpopulations - in terms of spectral type, luminosity class, and spatial location - in the field of view. Methods. We measured projected rotational velocities, 3e sin i, by means of a Fourier transform method and a profile fitting method applied to a set of isolated spectral lines. We also used an iterative deconvolution procedure to infer the probability density, P(3e), of the equatorial rotational velocity, 3e. Results. The distribution of 3e sin i shows a two-component structure: a peak around 80 km s1 and a high-velocity tail extending up to 600 km s^-1 This structure is also present in the inferred distribution P(3e) with around 80% of the sample having 0 <3e ≤ 300 km s^-1 and the other 20% distributed in the high-velocity region. The presence of the low-velocity peak is consistent with what has been found in other studies for late O- and early B-type stars. Conclusions. Most of the stars in our sample rotate with a rate less than 20% of their break-up velocity. For the bulk of the sample, mass loss in a stellar wind and/or envelope expansion is not efficient enough to significantly spin down these stars within the first few Myr of evolution. If massive-star formation results in stars rotating at birth with a large portion of their break-up velocities, an alternative braking mechanism, possibly magnetic fields, is thus required to explain the present-day rotational properties of the O-type stars in 30 Dor. The presence of a sizeable population of fast rotators is compatible with recent population synthesis computations that investigate the influence of binary evolution on the rotation rate of massive stars. Even though we have excluded stars that show significant radial velocity variations, our sample may have remained contaminated by post-interaction binary products. That the highvelocity tail may be populated primarily (and perhaps exclusively) by post-binary interaction products has important implications for the evolutionary origin of systems that produce gamma-ray bursts. © 2013 Author(s).

An extreme planetary system around HD 219828: one long-period super Jupiter to a hot-Neptune host star

Context. With about 2000 extrasolar planets confirmed, the results show that planetary systems have a whole range of unexpected properties. This wide diversity provides fundamental clues to the processes of planet formation and evolution. Aims: We present a full investigation of the HD 219828 system, a bright metal-rich star for which a hot Neptune has previously been detected. Methods: We used a set of HARPS, SOPHIE, and ELODIE radial velocities to search for the existence of orbiting companions to HD 219828. The spectra were used to characterise the star and its chemical abundances, as well as to check for spurious, activity induced signals. A dynamical analysis is also performed to study the stability of the system and to constrain the orbital parameters and planet masses. Results: We announce the discovery of a long period (P = 13.1 yr) massive (m sini = 15.1 MJup) companion (HD 219828 c) in a very eccentric orbit (e = 0.81). The same data confirms the existence of a hot Neptune, HD 219828 b, with a minimum mass of 21 M⊕ and a period of 3.83 days. The dynamical analysis shows that the system is stable, and that the equilibrium eccentricity of planet b is close to zero. Conclusions: The HD 219828 system is extreme and unique in several aspects. First, ammong all known exoplanet systems it presents an unusually high mass ratio. We also show that systems like HD 219828, with a hot Neptune and a long-period massive companion are more frequent than similar systems with a hot Jupiter instead. This suggests that the formation of hot Neptunes follows a different path than the formation of their hot jovian counterparts. The high mass, long period, and eccentricity of HD 219828 c also make it a good target for Gaia astrometry as well as a potential target for atmospheric characterisation, using direct imaging or high-resolution spectroscopy. Astrometric observations will allow us to derive its real mass and orbital configuration. If a transit of HD 219828 b is detected, we will be able to fully characterise the system, including the relative orbital inclinations. With a clearly known mass, HD 219828 c may become a benchmark object for the range in between giant planets and brown dwarfs.