On the Stability of Small-Scale Magnetic Elements in the Quiet Photospheric Network

Müller, R.; Moity, J.; Dollfus, Audouin; Montagné, M.; Vigneau, J.

doi:10.1007/978-94-015-9329-8_33

Cited by 17 publications

(19 citation statements)

References 21 publications

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“…In particular, Keller (1992) found that magnetic features larger than 0.4 arcsec in size tend to be darker than their surroundings. Muller et al (2000) and Zhang et al (1998) found that the bright filigree is related to magnetic features, but it is not generally cospatial. However, Fig.…”

Section: Resultsmentioning

confidence: 99%

“…Some previous works in the measurement of the magnetic field at high spatial resolution have been performed by different authors. Simultaneous direct observation of white light proxies and magnetic fields allowed them to establish the link between these two quantities for the solar flux tubes (Muller et al 2000;Keller 1992). Zhang et al (1998) found that most of the bright features such as filigree in photospheric filtergrams are related to corresponding magnetic features.…”

Section: Introductionmentioning

confidence: 99%

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High resolution solar magnetometry with the spectrograph of the Pic du Midi Turret Dome

Malherbe¹,

Roudier

Mein³

et al. 2004

A&A

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Abstract. We present the first results obtained with a new Ferroelectric Liquid Crystal (FLC) polarimeter operating with the spectrograph of the Pic du Midi Turret Dome, since September 2003. We observed the solar granulation around active region NOAA 0459 with the Multichannel Subtractive Double Pass (MSDP) operating mode and analysed the circular polarization of the Na D1 589.6 nm spectral line in terms of longitudinal magnetic fields in a 2D field of view (16 × 142 arcsec). Image quality was fairly good and limited to 0.4 arcsec due to the pixel sampling. This observation reveals the presence of magnetic concentrations of several hundred Gauss which are mainly located in the intergranular lanes. Data analysis performed at two different optical depths (line core and line wings) also suggests that magnetic lines are curved and diverge with increasing altitude.

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Section: Resultsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

High resolution solar magnetometry with the spectrograph of the Pic du Midi Turret Dome

Malherbe¹,

Roudier

Mein³

et al. 2004

A&A

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“…These have been well-studied at the atmospheric layers we sample, i.e., from the upper photosphere to the low chromosphere (e.g., Lites et al 1993;Wellstein et al 1998). They are connected to photospheric BPs (e.g., Riethmüller et al 2010) with concentrated kilo-Gauss, nearly vertical magnetic elements described by flux tubes (e.g., Spruit 1976;Solanki 1993;Yelles Chaouche et al 2009), and have been often referred to as MBPs (magnetic bright points; e.g., see Muller et al 2000;Möstl et al 2006) or GBPs (when identified in the G-band passband; e.g., Berger & Title 2001;Steiner et al 2001;Sánchez Almeida et al 2001Schüssler et al 2003;Shelyag et al 2004;Bovelet & Wiehr 2008).…”

Section: Introductionmentioning

confidence: 99%

Structure and dynamics of isolated internetwork Ca II H bright points observed by SUNRISE

Jafarzadeh

Solanki

Feller

et al. 2013

A&A

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Aims. We aim to improve our picture of the low chromosphere in the quiet-Sun internetwork by investigating the intensity, horizontal velocity, size and lifetime variations of small bright points (BPs; diameter smaller than 0.3 arcsec) observed in the Ca ii H 3968 Å passband along with their magnetic field parameters, derived from photospheric magnetograms. Methods. Several high-quality time series of disc-centre, quiet-Sun observations from the Sunrise balloon-borne solar telescope, with spatial resolution of around 100 km on the solar surface, have been analysed to study the dynamics of BPs observed in the Ca ii H passband and their dependence on the photospheric vector magnetogram signal.Results. Parameters such as horizontal velocity, diameter, intensity and lifetime histograms of the isolated internetwork and magnetic Ca ii H BPs were determined. Mean values were found to be 2.2 km s −1 , 0.2 arcsec (≈150 km), 1.48 I Ca and 673 s, respectively. Interestingly, the brightness and the horizontal velocity of BPs are anti-correlated. Large excursions (pulses) in horizontal velocity, up to 15 km s −1 , are present in the trajectories of most BPs. These could excite kink waves travelling into the chromosphere and possibly the corona, which we estimate to carry an energy flux of 310 W m −2 , sufficient to heat the upper layers, although only marginally. Conclusions. The stable observing conditions of Sunrise and our technique for identifying and tracking BPs have allowed us to determine reliable parameters of these features in the internetwork. Thus we find, e.g., that they are considerably longer lived than previously thought. The large velocities are also reliable, and may excite kink waves. Although these wave are (marginally) energetic enough to heat the quiet corona, we expect a large additional contribution from larger magnetic elements populating the network and partly also the internetwork.

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“…To date, many observations have achieved sub-0. 3 angular resolution and have resulted in measurements of magnetic element apparent size, brightness, field structure, dynamics, and evolution (Nisenson et al 2003;Berger & Title 2001;Muller et al 2000;Berger et al 1998b;van Ballegooijen et al 1998;Berger et al 1995;Muller et al 1994;Muller 1994;Keller 1992;Muller & Keil 1983;Muller 1983). All of these studies generally supported the idea that virtually all of the small-scale structure in active and quiet network regions was composed of filamentary flux tubes of kilogauss strength (we exclude here the internetwork regions which are thought to possess socalled "turbulent" flux with fields on the order of 10−100 G, Stenflo 1994).…”

Section: Introductionmentioning

confidence: 99%

Solar magnetic elements at 0$\farcs$1 resolution

Berger¹,

Voort²,

Löfdahl³

et al. 2004

A&A

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. We find that magnetic flux in this region as seen in both the magnetogram and the G-band image is typically structured into larger, amorphous, "ribbons" which are not resolved into individual flux tubes. The measured magnetic flux density in the ribbon structures ranges from 300 to 1500 Mx cm −2 , the higher values occurring at localized concentrations embedded within the ribbons. The Dopplergram indicates relative downflows associated with all magnetic elements with some indication that higher downflows occur adjacent to the peak magnetic flux location. The mean absolute magnetic flux density of the remnant plage network is about 130 Mx cm −2 ; in the lowest flux regions of the field-of-view, the mean absolute flux density is approximately 60 Mx cm −2 . Within these quiet regions we do not find evidence of pervasive kilo-gauss strength magnetic elements as seen in recent high resolution internetwork studies. In general, the observations confirm recent 3-dimensional numerical simulations which show that the magnetic field in high-density regions such as plage is concentrated in complex structures that are not generally composed of discrete magnetic flux tubes.

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On the Stability of Small-Scale Magnetic Elements in the Quiet Photospheric Network

Cited by 17 publications

References 21 publications

High resolution solar magnetometry with the spectrograph of the Pic du Midi Turret Dome

High resolution solar magnetometry with the spectrograph of the Pic du Midi Turret Dome

Structure and dynamics of isolated internetwork Ca II H bright points observed by SUNRISE

Solar magnetic elements at 0$\farcs$1 resolution

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