Precision Analysis of Evolved Stars. (arXiv:1903.05109v1 [astro-ph.SR])

Precision Analysis of Evolved Stars. (arXiv:1903.05109v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Ridgway_S/0/1/0/all/0/1">Stephen Ridgway</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Akeson_R/0/1/0/all/0/1">Rachel Akeson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baines_E/0/1/0/all/0/1">Ellyn Baines</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Creech_Eakman_M/0/1/0/all/0/1">Michelle Creech-Eakman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Boyajian_T/0/1/0/all/0/1">Tabetha Boyajian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Beck_E/0/1/0/all/0/1">Elvire De Beck</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dupree_A/0/1/0/all/0/1">Andrea Dupree</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gies_D/0/1/0/all/0/1">Doug Gies</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hinkle_K/0/1/0/all/0/1">Kenneth Hinkle</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Humphreys_E/0/1/0/all/0/1">Elizabeth Humphreys</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Humphreys_R/0/1/0/all/0/1">Roberta Humphreys</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Joyce_R/0/1/0/all/0/1">Richard Joyce</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Matthews_L/0/1/0/all/0/1">Lynn Matthews</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Monnier_J/0/1/0/all/0/1">John Monnier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Norris_R/0/1/0/all/0/1">Ryan Norris</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Roettenbacher_R/0/1/0/all/0/1">Rachael Roettenbacher</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stanghellini_L/0/1/0/all/0/1">Letizia Stanghellini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brumellaar_T/0/1/0/all/0/1">Theo ten Brumellaar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Belle_G/0/1/0/all/0/1">Gerard van Belle</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vlemmings_W/0/1/0/all/0/1">Wouter Vlemmings</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wheeler_J/0/1/0/all/0/1">J Craig Wheeler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+White_R/0/1/0/all/0/1">Russell White</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ziurys_L/0/1/0/all/0/1">Lucy Ziurys</a>

Evolved stars dominate galactic spectra, enrich the galactic medium, expand
to change their planetary systems, eject winds of a complex nature, produce
spectacular nebulae and illuminate them, and transfer material between binary
companions. While doing this, they fill the HR diagram with diagnostic loops
that write the story of late stellar evolution. Evolved stars sometimes release
unfathomable amounts of energy in neutrinos, light, kinetic flow, and
gravitational waves. During these late-life times, stars evolve complexly, with
expansion, convection, mixing, pulsation, mass loss. Some processes have
virtually no spatial symmetries, and are poorly addressed with low-resolution
measurements and analysis. Even a “simple” question as how to model mass loss
resists solution. However, new methods offer increasingly diagnostic tools.
Astrometry reveals populations and groupings. Pulsations/oscillations support
study of stellar interiors. Optical/radio interferometry enable 2-3d imagery of
atmospheres and shells. Bright stars with rich molecular spectra and velocity
fields are a ripe opportunity for imaging with high spatial and spectral
resolution, giving insight into the physics and modeling of later stellar
evolution.

Evolved stars dominate galactic spectra, enrich the galactic medium, expand
to change their planetary systems, eject winds of a complex nature, produce
spectacular nebulae and illuminate them, and transfer material between binary
companions. While doing this, they fill the HR diagram with diagnostic loops
that write the story of late stellar evolution. Evolved stars sometimes release
unfathomable amounts of energy in neutrinos, light, kinetic flow, and
gravitational waves. During these late-life times, stars evolve complexly, with
expansion, convection, mixing, pulsation, mass loss. Some processes have
virtually no spatial symmetries, and are poorly addressed with low-resolution
measurements and analysis. Even a “simple” question as how to model mass loss
resists solution. However, new methods offer increasingly diagnostic tools.
Astrometry reveals populations and groupings. Pulsations/oscillations support
study of stellar interiors. Optical/radio interferometry enable 2-3d imagery of
atmospheres and shells. Bright stars with rich molecular spectra and velocity
fields are a ripe opportunity for imaging with high spatial and spectral
resolution, giving insight into the physics and modeling of later stellar
evolution.

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