Searcharxiv⌕ Search
Home/Archive/arXiv

arXiv · 0812.4603

The magnetic field of the B3V star 16 Pegasi

H. F. Henrichs·C. Neiner·R. S. Schnerr·E. Verdugo·A. Alecian·C. Catala·F. Cochard·J. Gutiérrez·A. -L. Huat·J. Silvester·O. Thizy
View original source ↗Read source document ↗Export metadata ↓

Abstract

The Slowly Pulsating B3V star 16 Pegasi was discovered by Hubrig (2006) to be magnetic, based on low-resolution spectropolarimetric observations with FORS1 at the VLT. We have confirmed the presence of a magnetic field with new measurements with the spectropolarimeters Narval at TBL, France and Espadons at CFHT, Hawaii during 2007. The most likely period is about 1.44 d for the modulation of the field, but this could not be firmly established with the available data set. No variability has been found in the UV stellar wind lines. Although the star was reported once to show H alpha in emission, there exists at present no confirmation that the star is a Be star.

Explore related subjects

astro-ph

Keep this discovery

BibTeXRIS

H. F. Henrichs, C. Neiner, R. S. Schnerr, E. Verdugo, A. Alecian, C. Catala, F. Cochard, J. Gutiérrez, A. -L. Huat, J. Silvester, O. Thizy. 2008-12-25. The magnetic field of the B3V star 16 Pegasi. https://doi.org/10.1017/s1743921309030828

Cite the original work for its findings. Save a collection to share your selection of sources.

KEEP EXPLORING

Related papers

arXiv2017

Lecture notes on the formation and early evolution of planetary systems

These notes provide an introduction to the theory of the formation and early evolution of planetary systems. Topics covered include the structure, evolution and dispersal of protoplanetary disks; the formation of planetesimals, terrestrial and gas giant planets; and orbital evolution due to gas disk migration, planetesimal scattering, planet-planet interactions, and tides.

astro-ph↗
arXiv2017

Optimisation of the 3-body dynamics applied to extra-solar planetary systems

The body of work presented here revolves around the investigation of the existence and nature of extra-solar planetary systems. The fitting of stellar radial velocity time series data is attempted by constructing a model to quantify the orbital properties of a star-planetary system. This is achieved with the Planetary Orbit Fitting Process (POFP). Though specific to the investigated problem, the POFP is founded on two separate, more general ideas. One is a Solver producing the gravitational dynamics of a Three-Body system by integrating its Newtonian equations of motion. The other is an independent optimisation scheme. Both have been devised using MATLAB. Applying the optimisation to the Solver results in a realistic Three-Body dynamics that best describes the radial velocity data under the model-specific orbital-observational constraints. Combining these aspects also allows for the study of dynamical instability derived from interaction, which is reaffirmed as a necessary criterion for evaluating the fit. The validity of POFP solutions with respect to the observations and other models is discussed in this context. The underlying generality and fundamental principles demonstrate a larger frame of operation where problems in Physics and Mathematics can be solved with a multitude of techniques.

astro-ph↗
arXiv2017

Orbital Dynamics Of A Possible Second Planet In HD 17156

In this letter we report the possible existence of a second planet in the transiting extrasolar planet system HD 17156 and its interactive dynamics with the previously known planet. The analysis is achieved through the \POFP\ optimization software which is based on a full integration of the system's multiple-body Newtonian equations of motion. The two-planet solution yields a significantly improved fit to the previously published radial velocities. The two planets are strongly interacting and exchange angular momentum in a 5:1 mean motion resonance, yet remain stable as they mutually excite orbital eccentricities and periastron advances.

astro-ph↗