The magnetohydrodynamics angular rate sensor (MHD ARS) has received much attention for its ultra-low noise in ultra-broad bandwidth and its impact resistance in harsh environments; however, its poor performance at low frequency hinders its work in long time duration. The paper presents a modified MHD ARS combining Coriolis with MHD effect to extend the measurement scope throughout the whole ban...

A linear stability analysis was carried out for axial flow between a rotating porous inner cylinder and a concentric, stationary, porous outer cylinder when radial flow is present for several radius ratios. The radial Reynolds number, based on the radial velocity at the inner cylinder and the inner radius, was varied from 215 to 15, and the axial Reynolds number based on the mean axial velocity...

HD 45166 was selected as a candidate to the V Sagittae Class. It’s spectrum shows quite narrow emission lines of He, C, N, and O, possibly indicating a low inclination for the binary system. We performed high resolution and high stability Coudé spectroscopy in order to search for low amplitude radial velocity variations. The orbital period determined from the radial velocity curve is 0.357 days...

Context. RU Lup is a Classical T Tauri star with unusually strong emission lines, which has been interpreted as manifestations of accretion. Recently, evidence has accumulated that this star might have a variable radial velocity. Aims. We intended to investigate in more detail the possible variability in radial velocity using a set of 68 high-resolution spectra taken at the VLT (UVES), the AAT ...

Radial-velocity measurements and sine-curve fits to the orbital radial velocity variations are presented for ten close binary systems: OO Aql, CC Com, V345 Gem, XY Leo, AM Leo, V1010 Oph, V2612 Oph, XX Sex, W UMa, and XY UMa. Most of these binaries have been observed spectroscopically before, but our data are of higher quality and consistency than in the previous studies. While most of the stud...

We present observational radial velocity curves for 12 chromospherically active binary systems and individual measurements for a further 5 systems. These binaries are Six of our target binaries do not agree with published ephemerides or orbital parameters. We also present a rigourous derivation of the resolution limit for binary star cross-correlation radial velocities. Using synthetic spectral...

1Centre for Astrophysics Research, University of Hertfordshire, College Lane, Hatfield AL10 9AB, UK 2Department of Physics and Astronomy, University of Turku, Tuorla Observatory, Vňaisňalňantie 20, FI-21500 Piikkiňo, Finland 3Departamento de Astronomńõa, Universidad de Chile, Camino del Observatorio 1515, Las Condes, Santiago, Chile 4Astronomy Unit, School of Mathematical Sciences, Queen Mary U...