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Andic A.,BBSO
Proceedings of the International Astronomical Union | Year: 2010

Collision of the magnetic flux tubes in the Quiet Sun was proposed as one of the possible sources for the heating of the solar atmosphere (Furusawa and Sakai, 2000). The solar photosphere was observed using the New Solar Telescope ad Big Bear Solar Observatory. In TiO spectral line at 705.68 nm we approached resolution of 0.1. The horizontal plasma wave was observed spreading from the larger bright point. Shorty after this wave an increase in the oscillatory power appeared at the same location as the observed bright point. This behavior matches some of the results from the simulation of the collision of the two flux tubes with a weak current. © International Astronomical Union 2011. Source


Andic A.,BBSO | Chae J.,Seoul National University | Goode P.R.,BBSO
Proceedings of the International Astronomical Union | Year: 2010

Since photospheric bright points (BPs) were first observed, there has been a question as to how are they structured. Are they just single flux tubes or a bundle of the flux-tubes? Surface photometry of the quiet Sun (QS) has achieved resolution close to 0.1" with the New Solar Telescope at Big Bear Solar Observatory. This resolution allowed us to detect a richer spectrum of BPs in the QS. The smallest BPs we observed with TiO 705.68 nm were 0.13", and we were able to resolve individual components in some of the BPs clusters and ribbons observed in the QS, showing that they are composed of the individual BPs. Average size of observed BPs was 0.22". © International Astronomical Union 2011. Source


Andic A.,BBSO | Cao W.,BBSO | Goode P.R.,BBSO
Astrophysical Journal | Year: 2011

We detected peaks of oscillatory power at 3 and ∼6.5 minutes in the umbra of the central sunspot of the active region NOAA AR 10707 in data obtained in the near-infrared (NIR) continuum at 1565.7nm. The NIR data set captured umbral dynamics around 50km below the τ500 = 1 level. The umbra does not oscillate as a whole, but rather in distinct parts that are distributed over the umbral surface. The most powerful oscillations, close to a period of ∼6.5, do not propagate upward. We noted a plethora of large umbral dots (UDs) that persisted for ≥30minutes and stayed in the same locations. The peaks of oscillatory power above the detected UDs are located at 3 and 5minute oscillations, but are very weak in comparison with the oscillations of ∼6.5 minutes. © 2011. The American Astronomical Society. All rights reserved. Source


Andic A.,BBSO | Chae J.,BBSO | Chae J.,Seoul National University | Goode P.R.,BBSO | And 5 more authors.
Astrophysical Journal | Year: 2011

We detected 2.8 bright points (BPs) per Mm2 in the quiet Sun with the New Solar Telescope at Big Bear Solar Observatory, using the TiO 705.68 nm spectral line at an angular resolution 01 to obtain a 30 minute data sequence. Some BPs formed knots that were stable in time and influenced the properties of the granulation pattern around them. The observed granulation pattern within ∼3″ of knots presents smaller granules than those observed in a normal granulation pattern, i.e., around the knots a suppressed convection is detected. Observed BPs covered ∼5% of the solar surface and were not homogeneously distributed. BPs had an average size of 022, they were detectable for 4.28 minutes on average, and had an averaged contrast of 0.1% in the deep red TiO spectral line. © 2011. The American Astronomical Society. All rights reserved. Source

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