Volume 598, February 2017
|Number of page(s)||7|
|Published online||07 February 2017|
Dynamics of the photosphere along the solar cycle from SDO/HMI
1 Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse, CNRS, 14 avenue Édouard Belin, 31400 Toulouse, France
2 LESIA, Observatoire de Paris, Section de Meudon, 92195 Meudon, France
Received: 8 July 2016
Accepted: 2 November 2016
Context. As the global magnetic field of the Sun has an activity cycle, one expects to observe some variation of the dynamical properties of the flows visible in the photosphere.
Aims. We investigate the flow field during the solar cycle by analysing SDO/HMI observations of continuum intensity, Doppler velocity and longitudinal magnetic field.
Methods. We first picked data at disk center during 6 yr along the solar cycle with a 48-h time step in order to study the overall evolution of the continuum intensity and magnetic field. Then we focused on thirty 6-h sequences of quiet regions without any remnant of magnetic activity separated by 6 months, in summer and winter, when disk center latitude B0 is close to zero. The horizontal velocity was derived from the local correlation tracking technique over a field of view of 216.4 Mm × 216.4 Mm located at disk center.
Results. Our measurements at disk center show the stability of the flow properties between meso- and supergranular scales along the solar cycle.
Conclusions. The network magnetic field, produced locally at disk center independently from large scale dynamo, together with continuum contrast, vertical and horizontal flows, seem to remain constant during the solar cycle.
Key words: Sun: atmosphere / Sun: photosphere / Sun: magnetic fields
© ESO, 2017
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