I use a combination of multi-wavelength observations and modeling tools to study how exoplanetary systems form and evolve. Below is a subset of my publications. You can find a full list here.

  • Behmard, A., F. Dai, A. Howard, 2022, Stellar Companions To TESS Objects of Interest: A Test of Planet-Companion Alignment, AJ, 163, 160, ArXiv:2202.01798

  • Behmard, A., E. Petigura, A. Howard, 2019, Data-Driven Spectroscopy of Cool Stars at High Spectral Resolution, ApJ, 876, 68, ArXiv:1904.00094 

  • Behmard, A., D. Graninger, E. Fayolle, J. Bergner, K. Öberg, 2019, Desorption Kinetics and Binding Energies of Small Hydrocarbons, ApJ, 875, 73, ArXiv:1903.09720

Current research

I investigate the conditions of planet formation using stellar companions


Image credit: NASA/JPL-Caltech

Identifying and characterizing bound stellar companions (binary system, triples, etc.) can shed light on a planetary system's chemical and dynamical history. Stay tuned for results from ongoing research.

I model stellar spectra with data-driven/ML methods

synth_spectra-page-001 (1).jpg

Traditional methods of determining stellar properties (masses, radii, elemental abundances, etc.) based in spectral synthesis are bogged down by observational constraints or only work accurately within a subset of the HR diagram. Cool stars (<5200 K) are particularly difficult to model due to dense forests of molecular lines in their optical and NIR spectra.


We applied The Cannon, a data-driven/ML method to cool star spectra, with an eye towards correlating stellar parameters with characteristics of the planets they host. For more details, see our paper.

I study protoplanetary disk chemistry with laboratory methods 


Image credit: NASA/JPL-Caltech

Simple hydrocarbons are common in planet forming environments. Constraining their snowline locations allows us to make predictions of where these molecules exist in the ice vs. gas-phase during the different stages of star and planet formation, giving us a sense of the compositions of solid and gaseous material that contribute to forming planets.

I use laboratory experiments to constrain the desorption temperatures of hydrocarbons known to populate protoplanetary disks. Desorption temperatures can be used to derive binding energies, which in turn can be used to estimate snowline locations. For more details, see our paper.