REALIZATION OF ASYMPTOTICAL STABLE IN LARGE PROGRAM MOTION OF A GYROSTAT WITH VARIABLE INERTIA MOMENTS

2016 ◽  
Author(s):  
SERGEY BEZGLASNYI
Keyword(s):  
Program Motion ◽  
Large Program ◽  
Asymptotical Stable

The Galactic Center large program

2008 ◽  
Author(s):  
X. Haubois ◽  
R. Genzel ◽  
G. Perrin ◽  
S. Gillessen ◽  
T. Paumard ◽  
...  
Keyword(s):  
Galactic Center ◽  
Large Program

scholarly journals The VLT-FLAMES Tarantula Survey

2016 ◽  
Vol 12 (S329) ◽  
pp. 279-286
Author(s):  
Jorick S. Vink ◽  
C.J. Evans ◽  
J. Bestenlehner ◽  
C. McEvoy ◽  
O. Ramírez-Agudelo ◽  
...  
Keyword(s):  
Mass Loss ◽  
Main Sequence ◽  
Massive Stars ◽  
Mass Function ◽  
Large Magellanic Cloud ◽  
Initial Mass Function ◽  
Data Set ◽  
Large Program ◽  
Medium Resolution ◽  
Key Questions

AbstractWe present a number of notable results from the VLT-FLAMES Tarantula Survey (VFTS), an ESO Large Program during which we obtained multi-epoch medium-resolution optical spectroscopy of a very large sample of over 800 massive stars in the 30 Doradus region of the Large Magellanic Cloud (LMC). This unprecedented data-set has enabled us to address some key questions regarding atmospheres and winds, as well as the evolution of (very) massive stars. Here we focus on O-type runaways, the width of the main sequence, and the mass-loss rates for (very) massive stars. We also provide indications for the presence of a top-heavy initial mass function (IMF) in 30 Dor.

scholarly journals High gas-to-dust size ratio indicating efficient radial drift in the mm-faint CX Tauri disk

2019 ◽  
Vol 626 ◽  
pp. L2 ◽  
Author(s):  
S. Facchini ◽  
E. F. van Dishoeck ◽  
C. F. Manara ◽  
M. Tazzari ◽  
L. Maud ◽  
...  
Keyword(s):  
Near Infrared ◽  
Angular Resolution ◽  
Spectral Energy Distribution ◽  
Theoretical Models ◽  
Intensity Profile ◽  
Continuum Emission ◽  
Spectral Energy ◽  
High Angular Resolution ◽  
Sharp Drop ◽  
Large Program

The large majority of protoplanetary disks have very compact continuum emission (≲15 AU) at millimeter wavelengths. However, high angular resolution observations that resolve these small disks are still lacking, due to their intrinsically fainter emission compared with large bright disks. In this Letter we present 1.3 mm ALMA data of the faint disk (∼10 mJy) orbiting the TTauri star CX Tau at a resolution of ∼40 mas, ∼5 AU in diameter. The millimeter dust disk is compact, with a 68% enclosing flux radius of 14 AU, and the intensity profile exhibits a sharp drop between 10 and 20 AU, and a shallow tail between 20 and 40 AU. No clear signatures of substructure in the dust continuum are observed, down to the same sensitivity level of the DSHARP large program. However, the angular resolution does not allow us to detect substructures on the scale of the disk aspect ratio in the inner regions. The radial intensity profile closely resembles the inner regions of more extended disks imaged at the same resolution in DSHARP, but with no rings present in the outer disk. No inner cavity is detected, even though the disk has been classified as a transition disk from the spectral energy distribution in the near-infrared. The emission of 12CO is much more extended, with a 68% enclosing flux radius of 75 AU. The large difference of the millimeter dust and gas extents (> 5) strongly points to radial drift, and closely matches the predictions of theoretical models.

scholarly journals Discovery of a strong magnetic field in the rapidly rotating B2Vn star HR 7355

2010 ◽  
Vol 6 (S272) ◽  
pp. 204-205
Author(s):  
Mary E. Oksala ◽  
Gregg A. Wade ◽  
Wagner L. F. Marcolino ◽  
Jason H. Grunhut ◽  
David Bohlender ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Least Squares ◽  
Strong Magnetic Field ◽  
Type Star ◽  
Longitudinal Field ◽  
Rotational Period ◽  
V Band ◽  
Large Program ◽  
Differential Photometry

AbstractWe report on the detection of a strong, organized magnetic field in the helium-variable early B-type star HR 7355 using spectropolarimetric data obtained with ESPaDOnS on CFHT by the MiMeS large program. We also present results from new V-band differential photometry obtained with the CTIO 0.9m telescope. We investigate the longitudinal field, using a technique called Least-Squares Deconvolution (LSD), and the rotational period of HR 7355. These new observations strongly support the proposal that HR 7355 harbors a structured magnetosphere similar to that in the prototypical helium-strong star, σ Ori E.

scholarly journals High-resolution studies of the galactic equator region

1964 ◽  
Vol 20 ◽  
pp. 81-85 ◽  
Author(s):  
F. J. Kerr
Keyword(s):  
Fine Structure ◽  
Line Emission ◽  
Paper Tape ◽  
Great Variability ◽  
Line Profiles ◽  
Sample Group ◽  
Large Program ◽  
Point To Point ◽  
Adjacent Channels ◽  
The University

A large program of observations is being undertaken with the 210-foot telescope at Parkes, to study the fine structure of the 21-cm line emission in the region of the galactic equator. With the aid of a multi-channel receiver, H-line profiles have been obtained every 6 min of arc (i.e. every half-beamwidth) along the equator from lII=300 to 60°, and also from bII = −3 to +3° along a number of constant-longitude lines. The bandwidth of each channel of the receiver is equivalent to 8 · 0 km/sec, with a spacing of 7 · 0 km/sec between the centres of adjacent channels. The data have been recorded on punched paper tape, and the main reduction is being carried out on the SILLIAC computer of the University of Sydney. A sample group of profiles, illustrating the great variability from point to point, has been published previously (Kerr 1962b).

scholarly journals Asteroid (16) Psyche’s primordial shape: A possible Jacobi ellipsoid

2020 ◽  
Vol 638 ◽  
pp. L15 ◽  
Author(s):  
M. Ferrais ◽  
P. Vernazza ◽  
L. Jorda ◽  
N. Rambaux ◽  
J. Hanuš ◽  
...  
Keyword(s):  
Bulk Composition ◽  
Three Dimensional ◽  
Rotation Period ◽  
Data Sets ◽  
Similar Data ◽  
Small Deviations ◽  
3D Shape ◽  
Large Program ◽  
Solar System Object ◽  
Equilibrium Figures

Context. Asteroid (16) Psyche is the largest M-type asteroid in the main belt and the target of the NASA Psyche mission. It is also the only asteroid of this size (D >  200 km) known to be metal rich. Although various hypotheses have been proposed to explain the rather unique physical properties of this asteroid, a perfect understanding of its formation and bulk composition is still missing. Aims. We aim to refine the shape and bulk density of (16) Psyche and to perform a thorough analysis of its shape to better constrain possible formation scenarios and the structure of its interior. Methods. We obtained disk-resolved VLT/SPHERE/ZIMPOL images acquired within our ESO large program (ID 199.C-0074), which complement similar data obtained in 2018. Both data sets offer a complete coverage of Psyche’s surface. These images were used to reconstruct the three-dimensional (3D) shape of Psyche with two independent shape modeling algorithms (MPCD and ADAM). A shape analysis was subsequently performed, including a comparison with equilibrium figures and the identification of mass deficit regions. Results. Our 3D shape along with existing mass estimates imply a density of 4.20  ±  0.60 g cm−3, which is so far the highest for a solar system object following the four telluric planets. Furthermore, the shape of Psyche presents small deviations from an ellipsoid, that is, prominently three large depressions along its equator. The flatness and density of Psyche are compatible with a formation at hydrostatic equilibrium as a Jacobi ellipsoid with a shorter rotation period of ∼3h. Later impacts may have slowed down Psyche’s rotation, which is currently ∼4.2 h, while also creating the imaged depressions. Conclusions. Our results open the possibility that Psyche acquired its primordial shape either after a giant impact while its interior was already frozen or while its interior was still molten owing to the decay of the short-lived radionuclide 26Al.

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