Photospheric downflows observed with SDO/HMI, HINODE, and an MHD simulation

Result code in IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F21%3A00549022" target="_blank" >RIV/67985815:_____/21:00549022 - isvavai.cz</a>

Alternative codes found

RIV/00216208:11320/21:10436447

Result on the web

<a href="https://doi.org/10.1051/0004-6361/202040172" target="_blank" >https://doi.org/10.1051/0004-6361/202040172</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/202040172" target="_blank" >10.1051/0004-6361/202040172</a>

Result language

angličtina

Original language name

Photospheric downflows observed with SDO/HMI, HINODE, and an MHD simulation

Original language description

Downflows on the solar surface are suspected to play a major role in the dynamics of the convection zone, at least in its outer part. We investigate the existence of the long-lasting downflows whose effects influence the interior of the Sun but also the outer layers. We study the sets of Dopplergrams and magnetograms observed with Solar Dynamics Observatory and Hinode spacecrafts and an magnetohydrodynamic (MHD) simulation. All of the aligned sequences, which were corrected from the satellite motions and tracked with the differential rotation, were used to detect the long-lasting downflows in the quiet-Sun at the disc centre. To learn about the structure of the flows below the solar surface, the time-distance local helioseismology was used. The inspection of the 3D data cube (x, y, t) of the 24 h Doppler sequence allowed us to detect 13 persistent downflows. Their lifetimes lie in the range between 3.5 and 20 h with a sizes between 2 '' and 3 '' and speeds between -0.25 and -0.72 km s(-1). These persistent downflows are always filled with the magnetic field with an amplitude of up to 600 Gauss. The helioseismic inversion allows us to describe the persistent downflows and compare them to the other (non-persistent) downflows in the field of view. The persistent downflows seem to penetrate much deeper and, in the case of a well-formed vortex, the vorticity keeps its integrity to the depth of about 5 Mm. In the MHD simulation, only sub-arcsecond downflows are detected with no evidence of a vortex comparable in size to observations at the surface of the Sun. The long temporal sequences from the space-borne allows us to show the existence of long-persistent downflows together with the magnetic field. They penetrate inside the Sun but are also connected with the anchoring of coronal loops in the photosphere, indicating a link between downflows and the coronal activity. A links suggests that EUV cyclones over the quiet Sun could be an effective way to heat the corona.

Czech name

—

Czech description

—

Type

J_imp - Article in a specialist periodical, which is included in the Web of Science database

CEP classification

—

OECD FORD branch

10308 - Astronomy (including astrophysics,space science)

Project

<a href="/en/project/GA18-06319S" target="_blank" >GA18-06319S: Evolution of sunspots and active regions</a><br>

Continuities

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Publication year

2021

Confidentiality

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Name of the periodical

Astronomy & Astrophysics

ISSN

0004-6361

e-ISSN

1432-0746

Volume of the periodical

647

Issue of the periodical within the volume

March

Country of publishing house

FR - FRANCE

Number of pages

13

Pages from-to

A178

UT code for WoS article

000636753900001

EID of the result in the Scopus database

2-s2.0-85103694110