MAGNETIC LOOPS IN THE QUIET SUN

Wiegelmann, T; Solanki, S K; Barthol, P; Gandorfer, A; Borrero, J M; Schmidt, W; Pillet, V MartInez; Bonet, J A; Del Toro Iniesta, J C; Domingo, V; Knoelker, M

doi:10.1088/2041-8205/723/2/L185

Title: MAGNETIC LOOPS IN THE QUIET SUN

Full Record
Other Related Research

Abstract

We investigate the fine structure of magnetic fields in the atmosphere of the quiet Sun. We use photospheric magnetic field measurements from SUNRISE/IMaX with unprecedented spatial resolution to extrapolate the photospheric magnetic field into higher layers of the solar atmosphere with the help of potential and force-free extrapolation techniques. We find that most magnetic loops that reach into the chromosphere or higher have one footpoint in relatively strong magnetic field regions in the photosphere. Ninety-one percent of the magnetic energy in the mid-chromosphere (at a height of 1 Mm) is in field lines, whose stronger footpoint has a strength of more than 300 G, i.e., above the equipartition field strength with convection. The loops reaching into the chromosphere and corona are also found to be asymmetric in the sense that the weaker footpoint has a strength B < 300 G and is located in the internetwork (IN). Such loops are expected to be strongly dynamic and have short lifetimes, as dictated by the properties of the IN fields.

Authors:

Wiegelmann, T; Solanki, S K; Barthol, P; Gandorfer, A ^[1]; Borrero, J M; Schmidt, W ^[2]; Pillet, V MartInez; Bonet, J A ^[3]; Del Toro Iniesta, J C ^[4]; Domingo, V ^[5]; Knoelker, M ^[6]

Max-Planck-Institut fuer Sonnensystemforschung, Max-Planck-Str. 2, 37191 Katlenburg-Lindau (Germany)
Kiepenheuer-Institut fuer Sonnenphysik, Schoeneckstr. 6, 79104 Freiburg (Germany)
Instituto de Astrofisica de Canarias, C/Via Lactea s/n, 38200 La Laguna, Tenerife (Spain)
Instituto de Astrofisica de Andalucia (CSIC), Apartado de Correos 3004, 18080 Granada (Spain)
Grupo de Astronomia y Ciencias del Espacio, Universidad de Valencia, 46980 Paterna, Valencia (Spain)
High Altitude Observatory, National Center for Atmospheric Research Boulder, CO 80307 (United States)

Publication Date:: Wed Nov 10 00:00:00 EST 2010

OSTI Identifier:: 21457030

Resource Type:: Journal Article

Journal Name:: Astrophysical Journal Letters

Additional Journal Information:: Journal Volume: 723; Journal Issue: 2; Other Information: DOI: 10.1088/2041-8205/723/2/L185; Journal ID: ISSN 2041-8205

Country of Publication:: United States

Language:: English

Subject:: 79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ASYMMETRY; CHROMOSPHERE; CONVECTION; MAGNETIC FIELDS; PHOTOSPHERE; SPATIAL RESOLUTION; SUN; ATMOSPHERES; ENERGY TRANSFER; HEAT TRANSFER; MAIN SEQUENCE STARS; MASS TRANSFER; RESOLUTION; SOLAR ATMOSPHERE; STARS; STELLAR ATMOSPHERES

Citation Formats


                    Wiegelmann, T, Solanki, S K, Barthol, P, Gandorfer, A, Borrero, J M, Schmidt, W, Pillet, V MartInez, Bonet, J A, Del Toro Iniesta, J C, Domingo, V, Knoelker, M, and Title, A. M., E-mail: wiegelmann@mps.mpg.d. MAGNETIC LOOPS IN THE QUIET SUN.  United States: N. p., 2010. 
        Web.  doi:10.1088/2041-8205/723/2/L185.

Copy to clipboard


                    Wiegelmann, T, Solanki, S K, Barthol, P, Gandorfer, A, Borrero, J M, Schmidt, W, Pillet, V MartInez, Bonet, J A, Del Toro Iniesta, J C, Domingo, V, Knoelker, M, & Title, A. M., E-mail: wiegelmann@mps.mpg.d. MAGNETIC LOOPS IN THE QUIET SUN.  United States.  https://doi.org/10.1088/2041-8205/723/2/L185

Copy to clipboard


                    Wiegelmann, T, Solanki, S K, Barthol, P, Gandorfer, A, Borrero, J M, Schmidt, W, Pillet, V MartInez, Bonet, J A, Del Toro Iniesta, J C, Domingo, V, Knoelker, M, and Title, A. M., E-mail: wiegelmann@mps.mpg.d. 2010.  
        "MAGNETIC LOOPS IN THE QUIET SUN".  United States.  https://doi.org/10.1088/2041-8205/723/2/L185.

Copy to clipboard


                    
@article{osti_21457030,

  title        = {MAGNETIC LOOPS IN THE QUIET SUN},

  author       = {Wiegelmann, T and Solanki, S K and Barthol, P and Gandorfer, A and Borrero, J M and Schmidt, W and Pillet, V MartInez and Bonet, J A and Del Toro Iniesta, J C and Domingo, V and Knoelker, M and Title, A. M., E-mail: wiegelmann@mps.mpg.d},

  abstractNote = {We investigate the fine structure of magnetic fields in the atmosphere of the quiet Sun. We use photospheric magnetic field measurements from SUNRISE/IMaX with unprecedented spatial resolution to extrapolate the photospheric magnetic field into higher layers of the solar atmosphere with the help of potential and force-free extrapolation techniques. We find that most magnetic loops that reach into the chromosphere or higher have one footpoint in relatively strong magnetic field regions in the photosphere. Ninety-one percent of the magnetic energy in the mid-chromosphere (at a height of 1 Mm) is in field lines, whose stronger footpoint has a strength of more than 300 G, i.e., above the equipartition field strength with convection. The loops reaching into the chromosphere and corona are also found to be asymmetric in the sense that the weaker footpoint has a strength B < 300 G and is located in the internetwork (IN). Such loops are expected to be strongly dynamic and have short lifetimes, as dictated by the properties of the IN fields.},

  doi          = {10.1088/2041-8205/723/2/L185},

  url          = {https://www.osti.gov/biblio/21457030},
  journal      = {Astrophysical Journal Letters},

  issn         = {2041-8205},

  number       = 2,

  volume       = 723,

  place        = {United States},

  year         = {Wed Nov 10 00:00:00 EST 2010},

  month        = {Wed Nov 10 00:00:00 EST 2010}

}

Copy to clipboard

Journal Article:

https://doi.org/10.1088/2041-8205/723/2/L185

Other availability

Find in Google Scholar

Search WorldCat to find libraries that may hold this journal

Save / Share:

Export Metadata

Save to My Library

Similar records in OSTI.GOV collections:

The history of a quiet-sun magnetic element revealed by IMaX/SUNRISE

Journal Article Requerey, Iker; Del Toro Iniesta, Jose; Bellot Rubio, Luis; ... - Astrophysical Journal

Isolated flux tubes are considered to be fundamental magnetic building blocks of the solar photosphere. Their formation is usually attributed to the concentration of magnetic field to kG strengths by the convective collapse mechanism. However, the small size of the magnetic elements in quiet-Sun areas has prevented this scenario from being studied in fully resolved structures. Here, we report on the formation and subsequent evolution of one such photospheric magnetic flux tube, observed in the quiet Sun with unprecedented spatial resolution (0.''15-0.''18) and high temporal cadence (33 s). The observations were acquired by the Imaging Magnetograph eXperiment on board themore »« less
https://doi.org/10.1088/0004-637X/789/1/6
UNNOTICED MAGNETIC FIELD OSCILLATIONS IN THE VERY QUIET SUN REVEALED BY SUNRISE/IMaX

Journal Article Martinez Gonzalez, M; Asensio Ramos, A; Manso Sainz, R; ... - Astrophysical Journal Letters

We present observational evidence for oscillations of magnetic flux density in the quiet areas of the Sun. The majority of magnetic fields on the solar surface have strengths of the order of or lower than the equipartition field (300-500 G). This results in a myriad of magnetic fields whose evolution is largely determined by the turbulent plasma motions. When granules evolve they squash the magnetic field lines together or pull them apart. Here, we report on the periodic deformation of the shapes of features in circular polarization observed at high resolution with SUNRISE. In particular, we note that the areamore »« less
https://doi.org/10.1088/2041-8205/730/2/L37
Magneto-static Modeling from Sunrise/IMaX: Application to an Active Region Observed with Sunrise II

Journal Article Wiegelmann, T.; Solanki, S.; Barthol, P.; ... - Astrophysical Journal, Supplement Series

Magneto-static models may overcome some of the issues facing force-free magnetic field extrapolations. So far they have seen limited use and have faced problems when applied to quiet-Sun data. Here we present a first application to an active region. We use solar vector magnetic field measurements gathered by the IMaX polarimeter during the flight of the Sunrise balloon-borne solar observatory in 2013 June as boundary conditions for a magneto-static model of the higher solar atmosphere above an active region. The IMaX data are embedded in active region vector magnetograms observed with SDO /HMI. This work continues our magneto-static extrapolation approach,more »« less
https://doi.org/10.3847/1538-4365/AA582F
FULLY RESOLVED QUIET-SUN MAGNETIC FLUX TUBE OBSERVED WITH THE SUNRISE/IMAX INSTRUMENT

Journal Article Lagg, A; Solanki, S; Riethmueller, T; ... - Astrophysical Journal Letters

Until today, the small size of magnetic elements in quiet-Sun areas has required the application of indirect methods, such as the line-ratio technique or multi-component inversions, to infer their physical properties. A consistent match to the observed Stokes profiles could only be obtained by introducing a magnetic filling factor that specifies the fraction of the observed pixel filled with magnetic field. Here, we investigate the properties of a small magnetic patch in the quiet Sun observed with the IMaX magnetograph on board the balloon-borne telescope SUNRISE with unprecedented spatial resolution and low instrumental stray light. We apply an inversion techniquemore »« less
https://doi.org/10.1088/2041-8205/723/2/L164
WHAT IS THE SOURCE OF QUIET SUN TRANSITION REGION EMISSION?

Journal Article Schmit, D.; De Pontieu, Bart - Astrophysical Journal

Dating back to the first observations of the on-disk corona, there has been a qualitative link between the photosphere’s magnetic network and enhanced transition-temperature plasma emission. These observations led to the development of a general model that describes emission structures through the partitioning of the atmospheric volume with different magnetic loop geometries that exhibit different energetic equilibria. Does the internetwork produce transition-temperature emission? What fraction of network flux connects to the corona? How does quiet Sun emission compare with low-activity Sun-like stars? In this work, we revisit the canonical model of the quiet Sun, with high-resolution observations from the Interfacemore »« less
https://doi.org/10.3847/0004-637X/831/2/158

Similar Records