Bulletin of the American Physical Society
Mid-Atlantic Section 2022 Meeting
Volume 67, Number 20
Friday–Sunday, December 2–4, 2022; University Park, PA, Pennsylvania State University
Session B01: Space and Solar-Terrestrial Physics |
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Chair: Hugo Ayala, Pennsylvania State University Room: Pennsylvania State University Thomas 112 |
Friday, December 2, 2022 5:00PM - 5:35PM |
B01.00001: Turbulence in the young solar wind - Parker Solar Probe observations and global modeling Invited Speaker: Rohit Chhiber NASA's Parker Solar Probe (PSP) mission was launched in 2018, with the primary science objective of determining the structure and dynamics of the Sun's coronal magnetic field, understanding how the solar corona and wind are heated and accelerated, and determining the processes that accelerate energetic particles. The spacecraft's pioneering observations in the near-Sun space environment have led to novel insights, and raised new questions, regarding the nature and role of turbulence in the young solar wind. One topic of deep relevance is the nature of the transition from the magnetically structured, sub-Alfvénic inner corona into the super-Alfvénic, increasingly hydrodynamic young solar wind. This talk will first present an overview of the PSP mission and highlight some of its discoveries. We will then cover recent work exploring the transition from sub-Alfvénic to super-Alfvénic flow, using global magnetohydrodynamic modeling with turbulence transport, together with in-situ observations. We explore the possibility that, due to the influence of broadband turbulence, the critical Alfvénic transition takes place in fragmented and disconnected subvolumes within a general Alfvén critical zone. This picture stands in contrast to the conventional view of an Alfvén surface that separates simply connected regions. PSP has recently obtained the first measurements of sub-Alfvénic solar wind near the Sun, and we will end the presentation with a statistical analysis of magnetic turbulence observed in these regions. |
Friday, December 2, 2022 5:35PM - 6:10PM |
B01.00002: What are the planets made of, and how do we find out? Invited Speaker: David J Lawrence In the field of planetary science, we seek to understand how the planets formed and how they change over time. A key part of this understanding is finding out what the planets are made of, or more specifically, what is their elemental composition? In this talk, I will discuss a technique known as planetary nuclear spectroscopy. This technique uses gamma rays and neutrons to measure a planet’s elemental composition. I will first give an overview of the technique, and then take us on a tour of the solar system, stopping off at different planetary bodies where these measurements either have been or will be made. As part of this tour, I will discuss not only the measurements, but what is involved in building a space experiment and putting it into space. |
Friday, December 2, 2022 6:10PM - 6:22PM |
B01.00003: Proton and Electron Heating in Turbulent Magnetic Reconnection Joshua Goodwill, Yan Yang, William H Matthaeus, Sohom Roy, Fan Guo Magnetic Reconnection occurs when opposing magnetic fields collide and convert magnetic energy into kinetic and thermal energy. In a turbulent environment, magnetic reconnection modifies the cascade of energy of the system, and reconnection then produces a turbulent outflow, meaning that there must be a connection between the two processes. Studying reconnection in the environment of the solar wind, we can gain insight into the magnetic field structure in a turbulent environment. In previous studies the pressure strain has been shown to have a characteristic conversion between internal energy and fluid energy of the plasma at reconnection sites (Bandyopadhyay 2021). In particular, electrons are shown to be heated more than ions at these sites. A 2.5D VPIC (Vector Particle-in-Cell) simulation with solar-wind like parameters has been produced. The pressure strain calculations of the simulation have been completed and the magnetic fields along certain reconnection sites are displayed. In the future, reconnection sites can be found through calculating the saddle points of the magnetic vector potential (A). From there, the pressure strain analysis can be continued to calculate the heating of electrons and ions, which will then be compared to MMS data. |
Friday, December 2, 2022 6:22PM - 6:34PM |
B01.00004: Multi-messenger emission of Accretion Induce Collapse of White Dwarfs Luís F. L Micchi In his pivotal work, Chandrasekhar was able to show that an isolated White Dwarf (WD), in order to be stable, should have no more than ~1.4 solar masses, which is now known as the Chandrasekhar mass limit. As stars often occur in binary systems, it is common to find stars accreting mass from their companion. In this scenario, it should not come as a surprise if a WD is found to (temporarily) surpass the aforementioned limit. In this talk, I will discuss how this unstable WD will behave once the gravitational collapse is triggered. In particular, we will be interested in the case where the collapse is driven by an electron capture process, leading to an explosion, in an event named Accretion Induce Collapse. We will discuss the morphology of the multi-messenger signals of these sources with a larger focus on gravitational wave emission. |
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