Moving daily average of the hourly magnetic field values - the example of usage at Novosibirsk Observatory during 2011 (results and prospects)

The parameters of the equivalent central dipole calculated using hourly values of the magnetic field elements during 2011: the angular elements transformed to the hourly values of the geographic coordinates of the North magnetic pole and the intensity values transformed to local magnetic constant. Next step is the calculation of the daily mean values at every hour. This method applied to both current digital data and historical data presented as monthly tables of hourly values. The advantage of method is its ability to show the changes of the magnetic field independently from daily variation. Using of the “integrate” parameters (the magnetic pole coordinates and local magneto constant) allows detect the regional features of its variations. The features in the daily values compared with anomalous geological and geophysical events observed in the past and predicted in the near future.

MHD simulations of jet formation - protostellar jets & applications to AGN jets

Jet formation MHD simulations are presented considering a variety of model setups. The first approach investigates the interrelation between the disk magnetisation profile and jet collimation. Our results suggest (and quantify) that outflows launched from a very concentrated region at the inner disk tend to be weakly collimated. In the second approach, jet formation is investigated from a magnetic field configuration consisting of a stellar dipole superposed by a strong disk field. We find that the central dipole considerably de-collimates the disk wind. In addition, reconnection flares are launched in the interaction region of disk and stellar magnetic field, subsequently changing the outflow mass flux by factors of two. The time interval between flare ejection is about 1000 Keplerian periods - surprisingly similar to the observed time lag between jet knots. The third approach considers radiative pressure effects on jet collimation - an environment which is interesting mainly for outflows from massive young stars (but also for relativistic jets). Finally we present relativistic MHD simulations of jet formation from accretion disks extenting the previous non-relativistic approaches.

Beam Extraction From a Synchrotron Through a Magnetic Shield: Magnetic Measurements and Simulation of Efficiency

A new beam extraction scheme from a synchrotron is put forward. The main difference from other extraction schemes is the use of magnetic shields instead of a septum. The magnetic shield is a multi-layer copper-iron tube, which are located in the central dipole magnets of a pulsed chicane. Numerical simulations and experimental results for the field perturbation by magnetic shield are presented and compared. The calculation of extraction efficiency is presented.

A Beam Extraction Scheme From a Booster Synchrotron of Novosibirsk Sr Source

A beam extraction scheme from a cyclic accelerator is put forward. Its main difference from other schemes of extraction is the use of magnetic shields instead of a septum-magnet. Magnetic shields are located in the central dipole magnets of a pulsed chicane. The proposed scheme will be used for vertical extraction from a booster synchrotron to a storage ring in a new synchrotron radiation source in Novosibirsk.

Steady and Fluctuating Parts of Sun’s Internal Magnetic Field

We have modeled the ‘steady’ part of sun’s internal poloidal magnetic field in the form of a central dipole and a central hexapole with strengths (0.6±0.1) and embedded in an asymptotically uniform field Bo. A small deviation from isorotation seems to indicate:(i) a slow build-up of toroidal field near the base of the convection zone and (ii) presence of torsional MHD perturbations in the outer radiative core, with latitudinal structure and time scales which may be similar to those of solar activity.