In the present work we show robust indications of the existence of g modes in the Sun using 10 years of GOLF data. The present analysis is based on the exploitation of the collective properties of the predicted low-frequency (25 to 140 microHz) g modes: their asymptotic nature, which implies a quasi equidistant separation of their periods for a

In the present work we describe the formalism necessary to derive the properties of dark matter halos beyond 2 virial radii using the spherical collapse model (without shell crossing) and provide the framework for the theoretical prediction presented by Prada et al. We show in detail how to obtain within this model the probability distribution for

The spectral analyser of the Visible light Imager and Magnetograph (VIM) is a critical device whose concept is dependent on scientific requirements and technical trade-offs, which are directly driven by the nature of the mission. Here, we report on the choices that were made to fulfill the scientific needs, while constantly keeping an eye on

We have used observations made with the helioseismic instrument LOWL collected over ~6 years to carry out an independent study of the variations of the p-mode damping and excitation rates with solar activity. We observe significant variations in the mode height, mode width, and mode velocity power over a wide range of angular-degree values. Their

We present Chandra and XMM-Newton X-ray observations that monitor the neutron star cooling of the quasi-persistent neutron star X-ray transients KS 1731-260 and MXB 1659-29 for approximately 4 yr after these sources returned to quiescence from prolonged outbursts. In both sources the outbursts were long enough to significantly heat the neutron star

Aims.Our aim is to confirm the nature of the long period radial velocity measurements for β Gem first found by Hatzes & Cochran (1993). Methods: .We present precise stellar radial velocity measurements for the K giant star β Gem spanning over 25 years. An examination of the Ca II K emission, spectral line shapes from high resolution data (R = 210