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Thumbnail of Jupiter and Ring in Infrared from Webb
Why does Jupiter have rings? Jupiter's main ring was discovered in 1979 by NASA's passing Voyager 1 spacecraft, but its origin was then a mystery. Data from NASA's Galileo spacecraft that orbited Jupiter from 1995 to 2003, however, confirmed the hypothesis that this ring was created by meteoroid impacts on small nearby moons. As a small meteoroid strikes tiny Metis, for example, it will bore into the moon, vaporize, and explode dirt and dust off into a Jovian orbit. The featured image of Jupiter in infrared light by the James Webb Space Telescope shows not only Jupiter and its clouds, but this ring as well. Jupiter's Great Red Spot (GRS) -- in comparatively light color on the right, Jupiter's large moon Europa -- in the center of diffraction spikes on the left, and Europa's shadow -- next to the GRS -- are also visible. Several features in the image are not yet well understood, including the seemingly separated cloud layer on Jupiter's right limb. Celestial Surprise: What picture did APOD feature on your birthday? (post 1995)
Mount Timpanogos with sky above
Temperature: F
Rel. Humidity: %
Pressure: Inches Hg
Image for Nathan Powers, Updated labs and AAPT lab committee work
Dr. Powers initiated the effort to update BYU’s physics undergraduate lab curriculum in 2015. The revamped curriculum, aimed at teaching students how to construct knowledge from experiments.
Image for Study analyzes distant Kuiper Belt object with NASA's Hubble data
Using data from NASA's Hubble Space Telescope, a new study suggests that an object previously thought to be a binary system may be a rare triple system of orbiting bodies.
Image for BYU’s Rising Astronomers Take Center Stage at the Winter AAS Conference
In early January 2025, a group of 16 students from Brigham Young University’s Physics & Astronomy Department showcased their research at the prestigious American Astronomical Society (AAS) in National Harbor, Maryland.
Image for Acoustics group studies the roar of SpaceX's Starship
Acoustics faculty and students measure the thunderous noise of the world’s most powerful rocket, exploring its impact on communities and the environment.

Selected Publications

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By Yance Sun and Justin Peatross (et al.)
Abstract:

We investigate theoretically nonlinear Thomson scattering by multiple electrons ionized from individual atoms during a short high-intensity laser pulse. The emitted light is influenced by the distance that the electrons move apart from each other during the passage of the pulse, owing to coherence effects. We examine trajectories of electrons born from the same atom via successive ionizations as the laser pulse ramps up. While the overall trajectory of an individual electron is influenced by the ponderomotive force, we find that the separation between electrons arises mostly from stronger and differing initial drift velocities associated with the moment of ionization in the laser field. In the case of helium, we find that the separation between its two ionized electrons becomes appreciable (compared to emitted wavelengths) primarily along the dimension of laser linear polarization. This distorts the angular emission patterns of nonlinear Thomson scattering in comparison with emission from individual free electrons. Radiation scattered perpendicular to the laser polarization tends to add constructively, while radiation scattered along the direction of linear laser polarization tends to add incoherently. This effect becomes more pronounced for atoms with higher numbers of ionized electrons. The effect influences primarily the lower harmonic orders.

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By Joshua T. Mills, Peter K. Jensen, and Micah R. Shepherd
Abstract:

Vehicles in the upper atmosphere travel through increasingly rarefied media. As acoustic radiation is dependent upon its media, acoustic radiation losses of vibrating structures in lower density air are investigated. An aluminum Euler beam is placed in a vacuum chamber, supported by thin nylon wires at known nodal positions, according to the excited mode. These strings are laced across a large cavity in a small steel table, effectively minimizing losses due to boundary supports. An impulse hammer excites the beam into its flexural state, while a laser vibrometer measures the velocity response. Extraction of mechanical loss factors occurs as the vacuum pressure increases (atmospheric pressure decreases) in experimental increments, thus determining the dependence of acoustic radiation losses on the rarefied media. Analysis of experimental results is presented as a topic of discussion for vibrations of launch vehicles and satellites. Other inferences and inductions are also considered.

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By Alexandra M. Hopps-McDaniel and Tracianne B. Neilsen (et al.)
Abstract:

The very low-frequency noise from merchant ships provides a good broadband sound source to study the deep layers of the seabed. The nested striations that characterize ship time-frequency spectrograms contain unique acoustic features corresponding to where the waveguide invariant beta becomes infinite. In this dataset, these features occur at frequencies between 20 and 80 Hz, where pairs of modal group velocities become equal. The goal of this study is to identify these beta = infinity frequencies in ship noise spectrograms and use them to perform statistical inference for the deep layer sound speeds and thicknesses in the New England Mudpatch for a larger number of ships and acoustic arrays over a larger geographical region than previously studied. Marginal probability distributions of the data indicate that using singular points for a feature-based inversion yields an estimate of the sound speed and a limiting value for the thickness of the first deep layer. Heterogeneity is examined by correlating spatial variability of the deep layer sound speeds with ship tracks.

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By Scott G Call, Eric G Hintz, and Timothy D Morrell (et al.)
Abstract:

We present time-series near-infrared spectra for the classical Cepheid, CP Cephei, from the Astrophysical Research Consortium 3.5-m telescope and near-infrared spectrograph, TripleSpec, at Apache Point Observatory, NM, USA. Spectral observations were made at nine points through the minimum and partway up the ascending portion of the optical light curve for the star. Carbon monoxide (CO) was detected in absorption in the 2.3-$\mu$m region for each observation. We measured the strength of CO absorption using the 2-0 band head in the feature for each observation and confirm that the CO varies with pulsation. We show that these measurements follow the $(J-K)$ colour curve, confirming that temperature drives the destruction of CO. By obtaining convolved filter magnitudes from the spectral data we found that the effect of the CO feature on K magnitudes is small, unlike the CO feature in the mid-infrared at 4.5 $\mu$m. The dissociation of CO in the near-infrared spectra tracks with the effect seen in the mid-infrared photometric measurements of a similar Galactic Cepheid. Confirmation of the varying CO feature illustrates the need for further investigations into the related mid-infrared period-colour-metallicity relation in order to address the impact of Cepheid metallicities on the Hubble tension.

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Abstract:

We present 0.'' 22 resolution CO(2-1) observations of the circumnuclear gas disk in the local compact galaxy NGC 384 with the Atacama Large Millimeter/submillimeter Array (ALMA). While the majority of the disk displays regular rotation with projected velocities rising to 370 km s-1, the inner similar to 0.'' 5 exhibits a kinematic twist. We develop warped disk gas-dynamical models to account for this twist, fit those models to the ALMA data cube, and find a stellar mass-to-light ratio in the H band of M/L H = 1.34 +/- 0.01 [1 sigma statistical] +/- 0.02 [systematic] M circle dot/L circle dot and a supermassive black hole (BH) mass (M BH) of M BH =(7.26-0.48+0.43[1 sigma statistical]-1.00+0.55[systematic])x108M circle dot . In contrast to most previous dynamical M BH measurements in local compact galaxies, which typically found over-massive BHs compared to the local BH mass-bulge luminosity and BH mass-bulge mass relations, NGC 384 lies within the scatter of those scaling relations. NGC 384 and other local compact galaxies are likely relics of z similar to 2 red nuggets, and over-massive BHs in these relics indicate BH growth may conclude before the host galaxy stars have finished assembly. Our NGC 384 results may challenge this evolutionary picture, suggesting there may be increased scatter in the scaling relations than previously thought. However, this scatter could be inflated by systematic differences between stellar- and gas-dynamical measurement methods, motivating direct comparisons between the methods for NGC 384 and the other compact galaxies in the sample.

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We present new JWST observations of the nearby, prototypical edge-on, spiral galaxy NGC 891. The northern half of the disk was observed with NIRCam in its F150W and F277W filters. Absorption is clearly visible in the mid-plane of the F150W image, along with vertical dusty plumes that closely resemble the ones seen in the optical. A similar to 10 x 3 kpc(2) area of the lower circumgalactic medium (CGM) was mapped with MIRI F770W at 12 pc scales. Thanks to the sensitivity and resolution of JWST, we detect dust emission out to similar to 4 kpc from the disk, in the form of filaments, arcs, and super-bubbles. Some of these filaments can be traced back to regions with recent star formation activity, suggesting that feedback-driven galactic winds play an important role in regulating baryonic cycling. The presence of dust at these altitudes raises questions about the transport mechanisms at play and suggests that small dust grains are able to survive for several tens of million years after having been ejected by galactic winds in the disk-halo interface. We lay out several scenarios that could explain this emission: dust grains may be shielded in the outer layers of cool dense clouds expelled from the galaxy disk, and/or the emission comes from the mixing layers around these cool clumps where material from the hot gas is able to cool down and mix with these cool cloudlets. This first set of data and upcoming spectroscopy will be very helpful to understand the survival of dust grains in energetic environments, and their contribution to recycling baryonic material in the mid-plane of galaxies.