On January 17th I presented a talk entitled "Generating Buoyant Magnetic Loops in Convective Dynamos" at the 29th New Mexico Symposium at the National Radio Astronomy Observatory facility on the campus of New Mexico Tech in Socorro, New Mexico. This was the first time I had been to Socorro and to be honest I wasn't expecting much from the town. I was very pleasantly surprised by the town and the campus. New Mexico Tech is a very nice place to spend a day talking about astrophysics.
It was great to learn about things like the Jansky Very-Large Array, the CHILES survey, and variable stars studied by the Kepler Asteroseismic Consortium, but my personal favorite was hearing about the Magdelena Ridge Observatory. MRO is currently under construction on South Baldy mountain west of Socorro and when completed it will be 10 1.4 meter telescopes spaced over as much as 340 meters, which will be used together as an optical interferometer. By doing so it will be able to achieve an angular resolution equivalent to a single telescope with a diameter of 340 meters - or about 30 times bigger than the world's current largest optical telescope. When it comes online, MRO will be able to create resolved images of stars like our Sun - something that gets people like me very, very excited.
I focused on what we can do with the ASH code to simulate dynamo action and buoyant magnetic loops in sun-like stars. Below are a PDF copy of of the slides from my talk.
Showing posts with label Conferences. Show all posts
Showing posts with label Conferences. Show all posts
Wednesday, January 29, 2014
Tuesday, April 23, 2013
Conferences: Flux Emergence Worshop 2013
From April 15th through the 18th I attended the 5th edition of the Flux Emergence Workshop in Nice, France. I also attended the 4th edition of FEW at the Space Sciences Lab in Berkeley, California in 2011. FEW is a fairly unique conference compared to others I have attended in that it is topically very focused and registration is capped at about 40 people. This allows every attendee to give a 35 minute presentation. Presentations are generally much more interactive than in other conferences. The audience members regularly interrupt talks with questions which often result in some extended discussion involving the speaker and several other people. Because the meeting is so small these tend to be very productive and focused discussions.
I presented a talk entitled "Modeling the Origin of Tilt, Twist, Active Longitudes, and More: Buoyant Loops in Global Convective Dynamos", which was focused on the statistical properties of the ensemble of buoyant magnetic loops from my convective dynamo simulation (see papers here and here). One of the very interesting topics discussed at length concerns twist in sunspots. Previous simulations have indicated that buoyant magnetic loops need to be twisted in order to coherently rise through the solar convection zone. Measuring the twist in real sunspots is difficult and requires vector magnetograms which are only now becoming widely available, but observations seem to indicate that sunspots have an order of magnitude less twist on average than the minimum required by previous simulations. My simulated buoyant loops show a wide variety of amounts of twist and, on average, even slightly less than what is observed at the solar surface.
The histogram above shows the distribution of twists in my convective dynamo simulation (case S3) with a best-fit Gaussian distribution over-plotted in the black dashed curve. The vertical red dashed line shows the average twist observed in sunspots. Previous simulations have required a minimum twist rate on the order of +/-3 in these units. If the question is "Is twist required for the coherent rise of buoyant magnetic structures, or is it merely acquired from the dynamo generation mechanism?", the answer appears to be the latter.
It was a great conference and at a particularly beautiful location. The venue was Masion du Seminaires in Nice. As you can see from the pictures below, it was a spectacular venue.
The next FEW will be in Boulder in 2015 and I am already excited to attend.
I presented a talk entitled "Modeling the Origin of Tilt, Twist, Active Longitudes, and More: Buoyant Loops in Global Convective Dynamos", which was focused on the statistical properties of the ensemble of buoyant magnetic loops from my convective dynamo simulation (see papers here and here). One of the very interesting topics discussed at length concerns twist in sunspots. Previous simulations have indicated that buoyant magnetic loops need to be twisted in order to coherently rise through the solar convection zone. Measuring the twist in real sunspots is difficult and requires vector magnetograms which are only now becoming widely available, but observations seem to indicate that sunspots have an order of magnitude less twist on average than the minimum required by previous simulations. My simulated buoyant loops show a wide variety of amounts of twist and, on average, even slightly less than what is observed at the solar surface.
The histogram above shows the distribution of twists in my convective dynamo simulation (case S3) with a best-fit Gaussian distribution over-plotted in the black dashed curve. The vertical red dashed line shows the average twist observed in sunspots. Previous simulations have required a minimum twist rate on the order of +/-3 in these units. If the question is "Is twist required for the coherent rise of buoyant magnetic structures, or is it merely acquired from the dynamo generation mechanism?", the answer appears to be the latter.
It was a great conference and at a particularly beautiful location. The venue was Masion du Seminaires in Nice. As you can see from the pictures below, it was a spectacular venue.
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| View of Masion du Seminaires in Nice, France from the Mediterranean See. |
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| View of Nice and the Mediterranean See from a room like mine at the conference hotel. |
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