Response of the solar atmosphere to magnetic field evolution in a coronal hole region

AbstractNOAA 11035 was a highly sheared active region that appeared in December 2009 early in the new activity cycle. The leading polarity sunspot developed a highly unusual feature in its penumbra, an opposite polarity pore with a strong magnetic field in excess of 3500 G along one edge, which persisted for several days during the evolution of the region. This region was well observed by both space- and ground-based observatories, including Hinode, FIRS, TRACE, and SOHO. These observations, which span wavelength and atmospheric regimes, provide a complete picture of this unusual feature which may constitute a force-free magnetic field in the photosphere which is produced by the reconnection of magnetic loops low in the solar atmosphere.

Download Full-text

Magnetic field evolution in accreting white dwarfs

Monthly Notices of the Royal Astronomical Society ◽

10.1046/j.1365-8711.2002.05434.x ◽

2002 ◽

Vol 333 (3) ◽

pp. 589-602 ◽

Cited By ~ 48

Author(s):

A. Cumming

Keyword(s):

Magnetic Field ◽

White Dwarfs ◽

Field Evolution

Download Full-text

Photospheric magnetic field of an eroded-by-solar-wind coronal mass ejection

Proceedings of the International Astronomical Union ◽

10.1017/s1743921317001077 ◽

2016 ◽

Vol 12 (S327) ◽

pp. 67-70

Author(s):

J. Palacios ◽

C. Cid ◽

E. Saiz ◽

A. Guerrero

Keyword(s):

Magnetic Field ◽

Solar Wind ◽

Coronal Mass Ejection ◽

Coronal Hole ◽

Interplanetary Medium ◽

Flux Rope ◽

Magnetic Characteristics ◽

Interplanetary Coronal Mass Ejection ◽

Fast Wind ◽

Mass Ejection

AbstractWe have investigated the case of a coronal mass ejection that was eroded by the fast wind of a coronal hole in the interplanetary medium. When a solar ejection takes place close to a coronal hole, the flux rope magnetic topology of the coronal mass ejection (CME) may become misshapen at 1 AU as a result of the interaction. Detailed analysis of this event reveals erosion of the interplanetary coronal mass ejection (ICME) magnetic field. In this communication, we study the photospheric magnetic roots of the coronal hole and the coronal mass ejection area with HMI/SDO magnetograms to define their magnetic characteristics.

Download Full-text

Ages of radio pulsar: long-term magnetic field evolution

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/sty2945 ◽

2018 ◽

Vol 482 (3) ◽

pp. 3415-3425 ◽

Cited By ~ 5

Author(s):

Andrei P Igoshev

Keyword(s):

Magnetic Field ◽

Radio Pulsar ◽

Field Evolution

Download Full-text

Observations of magnetic and kinetic helicity proxies

Proceedings of the International Astronomical Union ◽

10.1017/s1743921313002160 ◽

2012 ◽

Vol 8 (S294) ◽

pp. 13-24

Author(s):

Hongqi Zhang

Keyword(s):

Magnetic Field ◽

Velocity Field ◽

Magnetic Fields ◽

Solar Atmosphere ◽

Active Regions ◽

Solar Dynamo ◽

Magnetic Helicity ◽

Vector Magnetograms ◽

Topological Configuration ◽

The Relationship

AbstractThe helicity is important to present the basic topological configuration of magnetic field in solar atmosphere. The distribution of magnetic helicity in solar atmosphere is presented by means of the observational (vector) magnetograms. As the kinetic helicity in the solar subatmosphere can be inferred from the velocity field based on the technique of the helioseismology and used to compare with the magnetic helicity in the solar atmosphere, the observational helicities provide the important chance for the confirmation on the generation of magnetic fields in the subatmosphere and solar dynamo models also. In this paper, we present the observational magnetic and kinetic helicity in solar active regions and corresponding questions, except the relationship with solar eruptive phenomena.

Download Full-text