Bay Area Environmental Research Institute

The planetary boundary layer confines moisture, turbulence, and locally emitted air pollutants, thus accurately discerning the height of this layer is important for constraining pollutant transport and distribution and improved regional weather and climate forecasting. Traditional methods of boundary layer height (BLH) determination rely on radiosonde measurements of potential temperature profiles. However, these sounding measurements lack the instrumentation needed to characterize the chemical composition of the boundary layer that can be provided by larger airborne platforms. In 2024, the NASA DC-8 flew over the Philippines, South Korea, Taiwan, and Thailand during the Airborne and Satellite Investigation of Asian Air Quality (ASIA-AQ) campaign. Measurements during this campaign included an extensive array of gas, particulate, and meteorological measurements. We will present results of a turbulence-based method using 3D winds to determine the boundary layer height across DC-8 vertical flight profiles, including missed approaches at urban airports. The results from this method were used to develop a boundary layer flag for the campaign, and the computed DC-8 BLHs were compared to mixed layer heights determined by an airborne-based LIDAR system.

The stratosphere is often considered to be dynamically stable with limited vertical exchange; however, episodic deep convection can even transport tropospheric air masses into the upper troposphere (UT) and even across the tropopause into lower stratosphere (LS). We deployed a newly developed airborne single particle mass spectrometer, Particle Analysis by Laser Mass Spectrometry – Next Generation (PALMS-NG), aboard a NASA ER-2 stratospheric aircraft to characterize aerosol particles in the UTLS during the Dynamics and Chemistry of the Summer Stratosphere (DCOTSS) mission. Here, we present observations revealing substantial perturbations of the stratospheric aerosol layer during an active convection and wildfire season in 2022.We show that carbonaceous–sulfate particles of tropospheric origin account for up to 90% of stratospheric particles with physical diameters between 0.1 and 1.5 µm within an approximately 4 km layer above the tropopause. Approximately 43% of these stratospheric carbonaceous–sulfate particles are directly attributed to biomass burning. The injected particles are chemically complex and organic-rich, and some exhibit internally mixed signatures containing both tropospheric and stratospheric components.Our observations further demonstrate that biomass-burning-related aerosols do not remain chemically unchanged following injections into the stratosphere. Instead, they undergo chemical mixing with stratospheric components, indicating a pronounced perturbation of the stratospheric aerosol layer driven by convective transport.These results highlight the coupling between dynamics and chemistry in modulating UTLS aerosol populations. As wildfire frequency and intensity increase alongside enhanced deep convection in a warming climate, convective delivery of biomass-burning products to the stratosphere may become increasingly important, with implications for ozone chemistry and radiative forcing.

Abstract Stratosphere‐troposphere exchange (STE) plays a crucial role in Earth's climate; however, the significance of small‐scale processes such as midlatitude convection to global STE remains understudied. Midlatitude tropopause‐overshooting convection is especially important to climate because it can enhance stratospheric water vapor, which has its greatest radiative forcing sensitivity in the extratropical lower stratosphere. Thus, it is essential to understand what factors influence the strength and prevalence of overshooting storms and associated STE. The U.S. Dynamics and Chemistry of the Summer Stratosphere (DCOTSS) field campaign during 2021 and 2022 was the first large‐scale airborne primarily focused on sampling stratospheric impacts from overshooting convection. Our research utilizes the extensive DCOTSS data set in combination with radar, satellite, and environmental observations to investigate relationships between observed stratosphere composition change and storm and environmental characteristics. Our results demonstrate greater magnitudes of STE for above‐anvil cirrus plume (AACP)‐producing storms and mesoscale convective systems (MCSs). In addition, the most extreme enhancements in water vapor and other tropospheric gases occur where the tropopause height is low and the depth of overshooting is high, especially for AACP‐producing storms. We also investigate the impact of storm and environmental characteristics on pathways for hydration (air mass transport and mixing vs. ice sublimation), finding that they also modulate the frequencies of each process at different altitudes. Namely, mixing is found to be most prevalent in AACP‐producing storms and MCSs, which can help explain transport differences between water vapor and other gases.

<strong class="journal-contentHeaderColor">Abstract.</strong> Aerosols in the upper troposphere play an important role in Earth&rsquo;s radiative balance and atmospheric composition. Satellite observations have revealed a recurrent enhancement of aerosol extinction coefficient (AEC) in the upper troposphere and near the tropopause over the Asian summer monsoon (ASM) anticyclone (ASMA) region during July&ndash;August. However, substantial uncertainties remain regarding (i) the influence of ASM dynamics and climate variability on these aerosols, (ii) the extent to which the upper-tropospheric aerosol trends reflect changes in surface pollutant emissions, and (iii) the ability of global models to simulate aerosol amounts, variability, and key controlling processes in the upper-tropospheric ASMA region. Here, we present results from an AeroCom-coordinated global multi-model study addressing these issues. Using simulations from nine models for 2000&ndash;2018, we find large inter-model differences in non-volcanic AEC over the upper-tropospheric ASMA region, with coefficients of variation ranging from 64 % to 86 %. Approximately half of this spread is attributable to differences in transport and wet removal processes, as diagnosed using common tracers, with discrepancies in wet removal contributing about eight times more than those associated with transport. The multi-model ensemble indicates an overall increase in non-volcanic AEC over the past two decades, consistent with rising anthropogenic emissions in Asia, while interannual variability is linked to climate variability as represented by the Multivariate ENSO Index. Through comparison with satellite observations, we further identify persistent model deficiencies, particularly in the representation of volcanic aerosols, and highlight priorities for future coordinated model developments and evaluation.

ABSTRACT Beyond orbital periods of 10 d, there is a dearth of known transiting gas giants. On longer orbits, planets are less affected by their host star, and become ideal probes of planet formation, migration, and evolution. We report the discovery of a long-period Neptune and two Saturns, each initially identified as single transits in the TESS (Transiting Exoplanet Survey Satellite) photometry, and solved through additional transits from ground-based follow-up photometric observations by NGTS (Next Generation Transit Survey) and ASTEP (Antarctic Search for Transiting ExoPlanets). High-resolution radial velocity mass measurements using CORALIE and HARPS (High Accuracy Radial Velocity Planet Searcher) confirm their planetary nature. From joint modelling of the photometric and spectroscopic data, we determine an orbital period of $43.12655_{-0.00017}^{+0.00012}~$ d, radius of $3.65\pm 0.22~\mathrm{R_{\hbox{$\oplus $}}}$, and mass of $19.1_{-4.5}^{+4.9}~\mathrm{M_{\hbox{$\oplus $}}}$ for NGTS-34 b, making it one of the longest period well-characterized transiting Neptunes. Orbiting a late F-type star, bright in the K band (Kmag$~\simeq 7.9$), it is amenable for cool atmosphere studies using James Webb Space Telescope or Ariel (Atmospheric Remote-sensing Infrared Exoplanet Large). TOI-4940 b is a small Saturn on a $25.867811_{-0.000056}^{+0.000058}~$ d orbit with a radius of $6.61\pm 0.37~\mathrm{R_{\hbox{$\oplus $}}}$ and an upper mass limit $&amp;lt; 89~\mathrm{M_{\hbox{$\oplus $}}}$. NGTS-35 b(=TOI-6669 b) is a larger Saturn on a $25.241192\pm 0.000022~$ d, moderately eccentric orbit ($e = 0.192_{-0.033}^{+0.037}$), with a radius of $10.90\pm 0.65~\mathrm{R_{\hbox{$\oplus $}}}$ and a mass of $152_{-19}^{+22}~\mathrm{M_{\hbox{$\oplus $}}}$. With an assumed albedo $A=0.3$, each of these planets has an equilibrium temperature below 700 K, with NGTS-35 b especially cold at $450~$ K. These three giants add to the small but growing population of long-period planets that can further our understanding of planet formation mechanisms.

Context . Super-Earths and mini-Neptunes are missing from our Solar System, yet they appear to be the most abundant planetary types in our Galaxy. A detailed characterization of key planets within this population is important for understanding the formation mechanisms of rocky and gas giant planets and the diversity of planetary interior structures. Aims . In 2019, NASA’s TESS satellite found a transiting planet candidate in a 17.6-day orbit around the star TOI-283. We started radial velocity (RV) follow-up observations with ESPRESSO to obtain a mass measurement. Mass and radius are measurements critical for planetary classification and internal composition modeling. Methods . We used ESPRESSO spectra to derive the stellar parameters of the planet candidate host star TOI-283. We then performed a joint analysis of the photometric and RV data of this star, using Gaussian processes to model the systematic noise present in both datasets. Results . We find that the host is a bright K-type star ( d = 82.4 pc, T eff = 5213 ± 70 K, V = 10.4 mag) with a mass and radius of M ⋆ = 0.80 ± 0.01 M ⊙ and R ⋆ = 0.85 ± 0.03 R ⊙ . The planet has an orbital period of P = 17.617 days, a size of R p = 2.34 ± 0.09 R ⊕ , and a mass of M p = 6.54 ± 2.04 M ⊕ . With an equilibrium temperature of ~600 K and a bulk density of ρ p = 2.81 ± 0.93 g cm −3 , this planet is positioned in the mass-radius diagram where planetary models predict H 2 O- and H/He-rich envelopes. The ESPRESSO RV data also reveal a long-term trend that is probably related to the star’s activity cycle. Further RV observations are required to confirm whether this signal originates from stellar activity or another planetary body in the system.

<strong class="journal-contentHeaderColor">Abstract.</strong> The age of smoke, meaning the time elapsed since it was produced in a fire, is an important parameter for interpreting measurements of evolving smoke composition. This study describes the smoke age estimates developed for large plumes sampled in the 2019 NASA-NOAA FIREX-AQ field experiment. Smoke ages are computed using two methods and applied to observations from two aircraft: the NASA DC-8 and a NOAA Twin Otter. The first method uses measurements of mean horizontal wind speed, as observed by the sampling aircraft, and distance to the fire to provide a single age estimate for each plume-crossing performed by the aircraft. While this "mean-wind method" uses accurate wind measurements, it can be systematically biased by assumptions that plume rise time is negligible and that winds are homogeneous horizontally and in time during the plume transport. Wind inhomogeneities due to terrain effects and day-to-night transition, among other factors, affected some plumes during FIREX-AQ. The mean-wind method therefore performs best for short-range transport over level terrain with steady winds. The second method relies on upwind air parcel trajectories and plume rise computed with multiple high-resolution meteorological datasets. This "trajectory-based method" quantifies age uncertainty from the meteorological ensemble, plume rise speed, wind speed errors, and fire location. The second method also resolves age differences from the center to edge of a transect. Still, it is susceptible to errors in the meteorological model. With careful comparison of the simulated trajectories to smoke transport observed from geostationary satellite imagery described here, we filter out many trajectory errors and improve the smoke age estimates. The two age methods are strongly correlated (<em>R</em> = 0.93) for the periods during FIREX-AQ when both ages are available. The mean-wind age is systematically 14&thinsp;% younger than the trajectory-based age and the median absolute difference between them is 19&thinsp;% (23&thinsp;% for mean). The favorable agreement between the two age methods reflects that the mean-wind method was selectively applied to plumes with little wind variability. Trajectory-based ages are available for more of the FIREX-AQ smoke observations than the mean-wind ages. The median trajectory-based age uncertainty during FIREX-AQ is 24&thinsp;% and the mean uncertainty is 37&thinsp;%, due to a long-tailed distribution. The main source of age uncertainty is spread within the meteorological ensemble, followed by discrepancy between measured and modeled wind speed, then other factors like plume rise. The age uncertainty variable enables the user to identify periods with high or low confidence in the age estimate, thereby informing studies of smoke aging.

Abstract We needed to evaluate available orbital data of NASA’s Volatiles Investigating Polar Exploration Rover (VIPER) mission area in order to derive a variety of maps to help the science team identify scientifically interesting places for the rover to visit and to provide scientific context for our mission. Some of these maps also fulfilled engineering and mission design needs to enable safe and efficient landing and roving. We incorporated data from the Lunar Reconnaissance Orbiter Camera, the Lunar Orbital Laser Altimeter, the Mini-RF instrument, the Chandrayaan-2 Orbital High Resolution Camera, the Korean Pathfinder Lunar Orbiter’s Shadowcam, the Kaguya Spectral Profiler and Multiband Imager, and the Chandrayaan-1 Moon Mineralogy Mapper. We used a variety of techniques to build these maps, including stereogrammetry, shape-from-shading, ice stability depth and surface temperature calculations, and the horizon method for solar illumination and direct-to-Earth communications maps. Altogether, these maps allowed us to survey for boulders, evaluate features in permanently shadowed regions that VIPER might explore, provide mineralogic context for what VIPER’s instruments may learn, estimate the ages and radar properties of craters in the VIPER mission area, and evaluate the potential for gravity traverses with the rover. These data and techniques provided a rich set of information from which both the VIPER science team and engineering teams were able to draw in order to plan a safe landing and to plan a VIPER surface mission that will be both scientifically valuable and robust from an operational perspective.

WASP-80 b, a warm sub-Jovian (equilibrium temperature [Formula: see text]820 K, 0.5 Jupiter masses), presents an opportunity to characterize a rare gas giant exoplanet around a low-mass star. In addition, its moderate temperature enables its atmosphere to host a range of carbon and oxygen species (H2O, CH4, CO, CO2, NH3). In this paper, we present a panchromatic emission spectrum of WASP-80 b, the first gas giant around a late K/early M-dwarf star and the coolest planet for which the James Webb Space Telescope has obtained a complete emission spectrum spanning 2.4 to 12 [Formula: see text]m, including NIRCam F322W2 (2.4 to 4 [Formula: see text]m) and F444W (4 to 5 [Formula: see text]m), and MIRI LRS (5 to 12 [Formula: see text]m). We report confident detections of H2O, CH4, CO, and CO2, and a tentative detection of NH3. We estimate WASP-80 b's atmospheric metallicity and carbon-to-oxygen ratio and compare them with estimates for other gas giants. Despite the relative rarity of giant planets around low-mass stars, we find that WASP-80 b's composition is consistent with other hot gas giants, suggesting that the formation pathway of WASP-80 b may not be dissimilar from hot gas giants around higher-mass stars.