Bio

Laura joined the department of Geological Sciences in January 2019 as an Assistant Professor. Laura received her Bachelor's from Washington University in St. Louis in 2002. She remained for several years at Washington University as a research assistant in Earth and Planetary Sciences, where she studied planetary atmospheres and their formation. In 2011, Laura began graduate school at the Harvard-Smithsonian Center for Astrophysics and received her PhD in Astronomy in 2016. Her thesis work focused on volatile cycles on rocky exoplanets, metal-silicate differentiation and atmosphere formation. In fall of 2016, Laura joined the School of Earth and Space Exploration at Arizona State University as a postdoctoral scholar where she worked on projects related to the evolution of mantle oxidation state and magma ocean evolution, as well as volatile cycles on planetesimals as a member of the NASA Psyche team.

Academic Appointments

Honors & Awards

  • Gabilan Faculty Fellow, Stanford University (2020-2021)

Professional Education

  • PhD, Harvard University, Astronomy & Astrophysics (2016)
  • B.A., Washington University in St. Louis, Earth and Planetary Science (2002)

Contact

  • Academic
    lkschaef@stanford.edu
    University - Faculty Department: Department of Geological Sciences Position: Assistant Professor
    • Geological Sciences Department
    • 450 Serra Mall Bldg. 320 Rm.118
    • Stanford,  California  94305 

Additional Info

Links

Current Research and Scholarly Interests

I study atmosphere-interior exchange on rocky planets, both within our Solar System and beyond. I'm interested in the initial outgassed atmospheres of rocky planets and their evolution with time due to external factors and due to interaction with the solid planet. During planet formation, all the materials that make a planet are intimately mixed together, so the physical and chemical processes of accretion and differentiation can have long term effects on the composition of both the atmosphere and the interior. I study these early processes using a combination of magma ocean, atmospheric and internal structure models. The presence of extant magma oceans on some hot rocky exoplanets provide a window into the early planet differentiation processes of the Solar System.

In the Solar System, I have particular interest in understanding the atmospheric evolution of Venus and Jupiter's moon Io, which both may have experienced significant volatile loss, likely through very different mechanisms. These planets are excellent proxies for the rocky exoplanets that will be observable in the near-term with new telescopes like the James Webb Space Telescope.

I am also interested in understanding the conditions of early atmospheric formation that may help or hinder the origins of life both within the Solar System and on exoplanets. Long-term interactions of atmosphere and interior will also influence the stability of habitable conditions on rocky exoplanets and are therefore vital to understand as astronomical observations of these planets become more feasible.

2024-25 Courses

Stanford Advisees

All Publications

  • Toward a Self-consistent Evaluation of Gas Dwarf Scenarios for Temperate Sub-Neptunes ASTROPHYSICAL JOURNAL Rigby, F. E., Pica-Ciamarra, L., Holmberg, M., Madhusudhan, N., Constantinou, S., Schaefer, L., Deng, J., Lee, K. M., Moses, J. I. 2024; 975 (1)

    View details for DOI 10.3847/1538-4357/ad6c38

    View details for Web of Science ID 001343971800001

  • Ferric Iron Evolution During Crystallization of the Earth and Mars JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS Schaefer, L., Pahlevan, K., Elkins-Tanton, L. T. 2024; 129 (9)

    View details for DOI 10.1029/2023JE008262

    View details for Web of Science ID 001312695300001

  • Outgassing Composition of the Murchison Meteorite: Implications for Volatile Depletion of Planetesimals and Interior-atmosphere Connections for Terrestrial Exoplanets PLANETARY SCIENCE JOURNAL Thompson, M. A., Telus, M., Edwards, G., Schaefer, L., Dhaliwal, J., Dreyer, B., Fortney, J. J., Kim, K. 2023; 4 (10)

    View details for DOI 10.3847/PSJ/acf760

    View details for Web of Science ID 001145433800001

  • No thick carbon dioxide atmosphere on the rocky exoplanet TRAPPIST-1 c. Nature Zieba, S., Kreidberg, L., Ducrot, E., Gillon, M., Morley, C., Schaefer, L., Tamburo, P., Koll, D. D., Lyu, X., Acuña, L., Agol, E., Iyer, A. R., Hu, R., Lincowski, A. P., Meadows, V. S., Selsis, F., Bolmont, E., Mandell, A. M., Suissa, G. 2023

    Abstract

    Seven rocky planets orbit the nearby dwarf star TRAPPIST-1, providing a unique opportunity to search for atmospheres on small planets outside the Solar System1. Thanks to the recent launch of the James Webb Space Telescope (JWST), possible atmospheric constituents such as carbon dioxide (CO2) are now detectable2,3. Recent JWST observations of the innermost planet TRAPPIST-1 b showed that it is most probably a bare rock without any CO2 in its atmosphere4. Here we report the detection of thermal emission from the dayside of TRAPPIST-1 c with the Mid-Infrared Instrument (MIRI) on JWST at 15 µm. We measure a planet-to-star flux ratio of fp/f⁎ = 421 ± 94 parts per million (ppm), which corresponds to an inferred dayside brightness temperature of 380 ± 31 K. This high dayside temperature disfavours a thick, CO2-rich atmosphere on the planet. The data rule out cloud-free O2/CO2 mixtures with surface pressures ranging from 10 bar (with 10 ppm CO2) to 0.1 bar (pure CO2). A Venus-analogue atmosphere with sulfuric acid clouds is also disfavoured at 2.6σ confidence. Thinner atmospheres or bare-rock surfaces are consistent with our measured planet-to-star flux ratio. The absence of a thick, CO2-rich atmosphere on TRAPPIST-1 c suggests a relatively volatile-poor formation history, with less than [Formula: see text] Earth oceans of water. If all planets in the system formed in the same way, this would indicate a limited reservoir of volatiles for the potentially habitable planets in the system.

    View details for DOI 10.1038/s41586-023-06232-z

    View details for PubMedID 37337068

    View details for PubMedCentralID 5330437

  • A primordial atmospheric origin of hydrospheric deuterium enrichment on Mars EARTH AND PLANETARY SCIENCE LETTERS Pahlevan, K., Schaefer, L., Elkins-Tanton, L. T., Desch, S. J., Buseck, P. R. 2022; 595

    View details for DOI 10.1016/j.epsl.2022.117772

    View details for Web of Science ID 000859556800006

  • The effects of bulk composition on planetesimal core sulfur content and size ICARUS Bercovici, H. L., Elkins-Tanton, L. T., O'Rourke, J. G., Schaefer, L. 2022; 380

    View details for DOI 10.1016/j.icarus.2022.114976

    View details for Web of Science ID 000793268100005

  • The Air Over There: Exploring Exoplanet Atmospheres ELEMENTS Schaefer, L. K., Parmentier, V. 2021; 17 (4): 257-263

    View details for DOI 10.2138/gselements.17.4.257

    View details for Web of Science ID 000752611600009

  • Composition of terrestrial exoplanet atmospheres from meteorite outgassing experiments NATURE ASTRONOMY Thompson, M. A., Telus, M., Schaefer, L., Fortney, J. J., Joshi, T., Lederman, D. 2021

    View details for DOI 10.1038/s41550-021-01338-8

    View details for Web of Science ID 000640440900002

  • Water on Hot Rocky Exoplanets ASTROPHYSICAL JOURNAL LETTERS Kite, E. S., Schaefer, L. 2021; 909 (2)

    View details for DOI 10.3847/2041-8213/abe7dc

    View details for Web of Science ID 000629137000001

  • Atmosphere Origins for Exoplanet Sub-Neptunes ASTROPHYSICAL JOURNAL Kite, E. S., Fegley, B., Schaefer, L., Ford, E. B. 2020; 891 (2)

    View details for DOI 10.3847/1538-4357/ab6ffb

    View details for Web of Science ID 000521379000001

  • Observations, Meteorites, and Models: A Preflight Assessment of the Composition and Formation of (16) Psyche JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS Elkins-Tanton, L. T., Asphaug, E., Bell, J. F., Bercovici, H., Bills, B., Binzel, R., Bottke, W. F., Dibb, S., Lawrence, D. J., Marchi, S., Mccoy, T. J., Oran, R., Park, R. S., Peplowski, P. N., Polanskey, C. A., Prettyman, T. H., Russell, C. T., Schaefer, L., Weiss, B. P., Wieczorek, M. A., Williams, D. A., Zuber, M. T. 2020; 125 (3): e2019JE006296

    Abstract

    Some years ago, the consensus was that asteroid (16) Psyche was almost entirely metal. New data on density, radar properties, and spectral signatures indicate that the asteroid is something perhaps even more enigmatic: a mixed metal and silicate world. Here we combine observations of Psyche with data from meteorites and models for planetesimal formation to produce the best current hypotheses for Psyche's properties and provenance. Psyche's bulk density appears to be between 3,400 and 4,100 kg m-3. Psyche is thus predicted to have between ~30 and ~60 vol% metal, with the remainder likely low-iron silicate rock and not more than ~20% porosity. Though their density is similar, mesosiderites are an unlikely analog to bulk Psyche because mesosiderites have far more iron-rich silicates than Psyche appears to have. CB chondrites match both Psyche's density and spectral properties, as can some pallasites, although typical pallasitic olivine contains too much iron to be consistent with the reflectance spectra. Final answers, as well as resolution of contradictions in the data set of Psyche physical properties, for example, the thermal inertia measurements, may not be resolved until the NASA Psyche mission arrives in orbit at the asteroid. Despite the range of compositions and formation processes for Psyche allowed by the current data, the science payload of the Psyche mission (magnetometers, multispectral imagers, neutron spectrometer, and a gamma-ray spectrometer) will produce data sets that distinguish among the models.

    View details for DOI 10.1029/2019JE006296

    View details for Web of Science ID 000535277900007

    View details for PubMedID 32714727

    View details for PubMedCentralID PMC7375145

  • Probing space to understand Earth Nature Reviews Earth & Environment Lapôtre, M. G., O'Rourke, J. G., Schaefer, L. K., Siebach, K. L., Spalding, C., Tikoo, S. M., Wordsworth, R. D. 2020; 1: 170-181

    View details for DOI 10.1038/s43017-020-0029-y

  • The Composition of Rocky Planets Planetary Diversity: Rocky planet processes and their observational signatures Unterborn, C., Schaefer, L., Krijt, S. IOP Publishing. 2020: 5-1 - 5-52
  • Superabundance of Exoplanet Sub-Neptunes Explained by Fugacity Crisis ASTROPHYSICAL JOURNAL LETTERS Kite, E. S., Fegley, B., Schaefer, L., Ford, E. B. 2019; 887 (2)

    View details for DOI 10.3847/2041-8213/ab59d9

    View details for Web of Science ID 000518385900006

  • Hydrogen isotopic evidence for early oxidation of silicate Earth EARTH AND PLANETARY SCIENCE LETTERS Pahlevan, K., Schaefer, L., Hirschmann, M. M. 2019; 526

    View details for DOI 10.1016/j.epsl.2019.115770

    View details for Web of Science ID 000488417000009

  • Absence of a thick atmosphere on the terrestrial exoplanet LHS 3844b. Nature Kreidberg, L. n., Koll, D. D., Morley, C. n., Hu, R. n., Schaefer, L. n., Deming, D. n., Stevenson, K. B., Dittmann, J. n., Vanderburg, A. n., Berardo, D. n., Guo, X. n., Stassun, K. n., Crossfield, I. n., Charbonneau, D. n., Latham, D. W., Loeb, A. n., Ricker, G. n., Seager, S. n., Vanderspek, R. n. 2019

    Abstract

    Most known terrestrial planets orbit small stars with radii less than 60 per cent of that of the Sun1,2. Theoretical models predict that these planets are more vulnerable to atmospheric loss than their counterparts orbiting Sun-like stars3-6. To determine whether a thick atmosphere has survived on a small planet, one approach is to search for signatures of atmospheric heat redistribution in its thermal phase curve7-10. Previous phase curve observations of the super-Earth 55 Cancri e (1.9 Earth radii) showed that its peak brightness is offset from the substellar point (latitude and longitude of 0 degrees)-possibly indicative of atmospheric circulation11. Here we report a phase curve measurement for the smaller, cooler exoplanet LHS 3844b, a 1.3-Earth-radii world in an 11-hour orbit around the small nearby star LHS 3844. The observed phase variation is symmetric and has a large amplitude, implying a dayside brightness temperature of 1,040 ± 40 kelvin and a nightside temperature consistent with zero kelvin (at one standard deviation). Thick atmospheres with surface pressures above 10 bar are ruled out by the data (at three standard deviations), and less-massive atmospheres are susceptible to erosion by stellar wind. The data are well fitted by a bare-rock model with a low Bond albedo (lower than 0.2 at two standard deviations). These results support theoretical predictions that hot terrestrial planets orbiting small stars may not retain substantial atmospheres.

    View details for DOI 10.1038/s41586-019-1497-4

    View details for PubMedID 31427764

  • Magma oceans as a critical stage in the tectonic development of rocky planets PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL AND ENGINEERING SCIENCES Schaefer, L., Elkins-Tanton, L. T. 2018; 376 (2132)

    Abstract

    Magma oceans are a common result of the high degree of heating that occurs during planet formation. It is thought that almost all of the large rocky bodies in the Solar System went through at least one magma ocean phase. In this paper, we review some of the ways in which magma ocean models for the Earth, Moon and Mars match present-day observations of mantle reservoirs, internal structure and primordial crusts, and then we present new calculations for the oxidation state of the mantle produced during the magma ocean phase. The crystallization of magma oceans probably leads to a massive mantle overturn that may set up a stably stratified mantle. This may lead to significant delays or total prevention of plate tectonics on some planets. We review recent models that may help alleviate the mantle stability issue and lead to earlier onset of plate tectonics.This article is part of a discussion meeting issue 'Earth dynamics and the development of plate tectonics'.

    View details for DOI 10.1098/rsta.2018.0109

    View details for Web of Science ID 000446261300012

    View details for PubMedID 30275166

    View details for PubMedCentralID PMC6189560

  • Origin of Earth's Water: Chondritic Inheritance Plus Nebular Ingassing and Storage of Hydrogen in the Core JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS Wu, J., Desch, S. J., Schaefer, L., Elkins-Tanton, L. T., Pahlevan, K., Buseck, P. R. 2018; 123 (10): 2691–2712

    View details for DOI 10.1029/2018JE005698

    View details for Web of Science ID 000450621300012

  • Redox Evolution via Gravitational Differentiation on Low-mass Planets: Implications for Abiotic Oxygen, Water Loss, and Habitability ASTRONOMICAL JOURNAL Wordsworth, R. D., Schaefer, L. K., Fischer, R. A. 2018; 155 (5)

    View details for DOI 10.3847/1538-3881/aab608

    View details for Web of Science ID 000439356900003

  • PLANETARY SCIENCE A steamy proposal for Martian clays NATURE Schaefer, L. 2017; 552 (7683): 37–38

    View details for Web of Science ID 000417560500036

    View details for PubMedID 32080510

  • Thermodynamic Constraints on the Lower Atmosphere of Venus ACS EARTH AND SPACE CHEMISTRY Jacobson, N. S., Kulis, M., Radoman-Shaw, B., Harvey, R., Myers, D. L., Schaefer, L., Fegley, B. 2017; 1 (7): 422–30

    View details for DOI 10.1021/acsearthspacechem.7b00067

    View details for Web of Science ID 000411771600006

  • Redox States of Initial Atmospheres Outgassed on Rocky Planets and Planetesimals ASTROPHYSICAL JOURNAL Schaefer, L., Fegley, B. 2017; 843 (2)

    View details for DOI 10.3847/1538-4357/aa784f

    View details for Web of Science ID 000405278700020

  • Metal-silicate Partitioning and Its Role in Core Formation and Composition on Super-Earths ASTROPHYSICAL JOURNAL Schaefer, L., Jacobsen, S. B., Remo, J. L., Petaev, M. I., Sasselov, D. D. 2017; 835 (2)

    View details for DOI 10.3847/1538-4357/835/2/234

    View details for Web of Science ID 000401154800026

  • PREDICTIONS OF THE ATMOSPHERIC COMPOSITION OF GJ 1132b ASTROPHYSICAL JOURNAL Schaefer, L., Wordsworth, R. D., Berta-Thompson, Z., Sasselov, D. 2016; 829 (2)

    View details for DOI 10.3847/0004-637X/829/2/63

    View details for Web of Science ID 000385377200005

  • ATMOSPHERE-INTERIOR EXCHANGE ON HOT, ROCKY EXOPLANETS ASTROPHYSICAL JOURNAL Kite, E. S., Fegley, B., Schaefer, L., Gaidos, E. 2016; 828 (2)

    View details for DOI 10.3847/0004-637X/828/2/80

    View details for Web of Science ID 000384089000007

  • SOLUBILITY OF ROCK IN STEAM ATMOSPHERES OF PLANETS ASTROPHYSICAL JOURNAL Fegley, B., Jacobson, N. S., Williams, K. B., Plane, J. C., Schaefer, L., Lodders, K. 2016; 824 (2)

    View details for DOI 10.3847/0004-637X/824/2/103

    View details for Web of Science ID 000381912800039

  • A disintegrating minor planet transiting a white dwarf NATURE Vanderburg, A., Johnson, J., Rappaport, S., Bieryla, A., Irwin, J., Lewis, J., Kipping, D., Brown, W. R., Dufour, P., Ciardi, D. R., Angus, R., Schaefer, L., Latham, D. W., Charbonneau, D., Beichman, C., Eastman, J., McCrady, N., Wittenmyer, R. A., Wright, J. T. 2015; 526 (7574): 546–49

    Abstract

    Most stars become white dwarfs after they have exhausted their nuclear fuel (the Sun will be one such). Between one-quarter and one-half of white dwarfs have elements heavier than helium in their atmospheres, even though these elements ought to sink rapidly into the stellar interiors (unless they are occasionally replenished). The abundance ratios of heavy elements in the atmospheres of white dwarfs are similar to the ratios in rocky bodies in the Solar System. This fact, together with the existence of warm, dusty debris disks surrounding about four per cent of white dwarfs, suggests that rocky debris from the planetary systems of white-dwarf progenitors occasionally pollutes the atmospheres of the stars. The total accreted mass of this debris is sometimes comparable to the mass of large asteroids in the Solar System. However, rocky, disintegrating bodies around a white dwarf have not yet been observed. Here we report observations of a white dwarf--WD 1145+017--being transited by at least one, and probably several, disintegrating planetesimals, with periods ranging from 4.5 hours to 4.9 hours. The strongest transit signals occur every 4.5 hours and exhibit varying depths (blocking up to 40 per cent of the star's brightness) and asymmetric profiles, indicative of a small object with a cometary tail of dusty effluent material. The star has a dusty debris disk, and the star's spectrum shows prominent lines from heavy elements such as magnesium, aluminium, silicon, calcium, iron, and nickel. This system provides further evidence that the pollution of white dwarfs by heavy elements might originate from disrupted rocky bodies such as asteroids and minor planets.

    View details for DOI 10.1038/nature15527

    View details for Web of Science ID 000364026100044

    View details for PubMedID 26490620

  • THE PERSISTENCE OF OCEANS ON EARTH-LIKE PLANETS: INSIGHTS FROM THE DEEP-WATER CYCLE ASTROPHYSICAL JOURNAL Schaefer, L., Sasselov, D. 2015; 801 (1)

    View details for DOI 10.1088/0004-637X/801/1/40

    View details for Web of Science ID 000350488700040

  • THE ATMOSPHERES OF EARTHLIKE PLANETS AFTER GIANT IMPACT EVENTS ASTROPHYSICAL JOURNAL Lupu, R. E., Zahnle, K., Marley, M. S., Schaefer, L., Fegley, B., Morley, C., Cahoy, K., Freedman, R., Fortney, J. J. 2014; 784 (1)

    View details for DOI 10.1088/0004-637X/784/1/27

    View details for Web of Science ID 000335457000027

  • Atmospheric composition of Hadean-early Archean Earth: The importance of CO: Comment Schaefer, L., Fegley, B., Shaw, G. H. GEOLOGICAL SOC AMER INC. 2014: 29–31

    View details for DOI 10.1130/2014.2504(05)

    View details for Web of Science ID 000339191800006

  • VAPORIZATION OF THE EARTH: APPLICATION TO EXOPLANET ATMOSPHERES ASTROPHYSICAL JOURNAL Schaefer, L., Lodders, K., Fegley, B. 2012; 755 (1)

    View details for DOI 10.1088/0004-637X/755/1/41

    View details for Web of Science ID 000306909500041

  • COMPOSITIONS OF HOT SUPER-EARTH ATMOSPHERES: EXPLORING KEPLER CANDIDATES ASTROPHYSICAL JOURNAL LETTERS Miguel, Y., Kaltenegger, L., Fegley, B., Schaefer, L. 2011; 742 (2)

    View details for DOI 10.1088/2041-8205/742/2/L19

    View details for Web of Science ID 000296924700003

  • The extreme physical properties of the CoRoT-7b super-Earth ICARUS Leger, A., Grasset, O., Fegley, B., Codron, F., Albarede, F., Barge, P., Barnes, R., Cance, P., Carpy, S., Catalano, F., Cavarroc, C., Demangeon, O., Ferraz-Mello, S., Gabor, P., Griessmeier, J., Leibacher, J., Libourel, G., Maurin, A., Raymond, S. N., Rouan, D., Samuel, B., Schaefer, L., Schneider, J., Schuller, P. A., Selsis, F., Sotin, C. 2011; 213 (1): 1–11

    View details for DOI 10.1016/j.icarus.2011.02.004

    View details for Web of Science ID 000290190100001

  • ATMOSPHERIC CHEMISTRY OF VENUS-LIKE EXOPLANETS ASTROPHYSICAL JOURNAL Schaefer, L., Fegley, B. 2011; 729 (1)

    View details for DOI 10.1088/0004-637X/729/1/6

    View details for Web of Science ID 000287255300006

  • Earth's Earliest Atmospheres COLD SPRING HARBOR PERSPECTIVES IN BIOLOGY Zahnle, K., Schaefer, L., Fegley, B. 2010; 2 (10): a004895

    Abstract

    Earth is the one known example of an inhabited planet and to current knowledge the likeliest site of the one known origin of life. Here we discuss the origin of Earth's atmosphere and ocean and some of the environmental conditions of the early Earth as they may relate to the origin of life. A key punctuating event in the narrative is the Moon-forming impact, partly because it made Earth for a short time absolutely uninhabitable, and partly because it sets the boundary conditions for Earth's subsequent evolution. If life began on Earth, as opposed to having migrated here, it would have done so after the Moon-forming impact. What took place before the Moon formed determined the bulk properties of the Earth and probably determined the overall compositions and sizes of its atmospheres and oceans. What took place afterward animated these materials. One interesting consequence of the Moon-forming impact is that the mantle is devolatized, so that the volatiles subsequently fell out in a kind of condensation sequence. This ensures that the volatiles were concentrated toward the surface so that, for example, the oceans were likely salty from the start. We also point out that an atmosphere generated by impact degassing would tend to have a composition reflective of the impacting bodies (rather than the mantle), and these are almost without exception strongly reducing and volatile-rich. A consequence is that, although CO- or methane-rich atmospheres are not necessarily stable as steady states, they are quite likely to have existed as long-lived transients, many times. With CO comes abundant chemical energy in a metastable package, and with methane comes hydrogen cyanide and ammonia as important albeit less abundant gases.

    View details for DOI 10.1101/cshperspect.a004895

    View details for Web of Science ID 000282451000012

    View details for PubMedID 20573713

    View details for PubMedCentralID PMC2944365

  • Chemistry of atmospheres formed during accretion of the Earth and other terrestrial planets ICARUS Schaefer, L., Fegley, B. 2010; 208 (1): 438–48

    View details for DOI 10.1016/j.icarus.2010.01.026

    View details for Web of Science ID 000278838200036

  • Volatile element chemistry during metamorphism of ordinary chondritic material and some of its implications for the composition of asteroids ICARUS Schaefer, L., Fegley, B. 2010; 205 (2): 483–96

    View details for DOI 10.1016/j.icarus.2009.08.025

    View details for Web of Science ID 000274599400012

  • Cosmochemistry Fegley, B., Schaefer, L., Goswami, A., Reddy, B. E. SPRINGER. 2010: 347–77

    View details for DOI 10.1007/978-3-642-10352-0_7

    View details for Web of Science ID 000279940700007

  • CHEMISTRY OF SILICATE ATMOSPHERES OF EVAPORATING SUPER-EARTHS ASTROPHYSICAL JOURNAL LETTERS Schaefer, L., Fegley, B. 2009; 703 (2): L113–L117

    View details for DOI 10.1088/0004-637X/703/2/L113

    View details for Web of Science ID 000270014600005

  • Chemistry and Composition of Planetary Atmospheres Schaefer, L., Fegley, B., Zaikowski, L., Friedrich, J. M. AMER CHEMICAL SOC. 2008: 187–207

    View details for Web of Science ID 000290566000010

  • Outgassing of ordinary chondritic material and some of its implications for the chemistry of asteroids, planets, and satellites ICARUS Schaefer, L., Fegley, B. 2007; 186 (2): 462–83

    View details for DOI 10.1016/j.icarus.2006.09.002

    View details for Web of Science ID 000244081200013

  • Application of an equilibrium vaporization model to the ablation of chondritic and achondritic meteoroids Schaefer, L., Fegley, B. SPRINGER. 2005: 413–23

    View details for DOI 10.1007/s11038-005-9030-1

    View details for Web of Science ID 000236083500041

  • Silicon tetrafluoride on Io ICARUS Schaefer, L., Fegley, B. 2005; 179 (1): 252–58

    View details for DOI 10.1016/j.icarus.2005.05.020

    View details for Web of Science ID 000233550600015

  • Alkali and halogen chemistry in volcanic gases on Io ICARUS Schaefer, L., Fegley, B. 2005; 173 (2): 454–68

    View details for DOI 10.1016/j.icarus.2004.08.015

    View details for Web of Science ID 000227596700015

  • Predicted abundances of carbon compounds in volcanic gases on Io ASTROPHYSICAL JOURNAL Schaefer, L., Fegley, B. 2005; 618 (2): 1079–85

    View details for DOI 10.1086/426113

    View details for Web of Science ID 000226293800051

  • A thermodynamic model of high temperature lava vaporization on Io ICARUS Schaefer, L., Fegley, B. 2004; 169 (1): 216–41

    View details for DOI 10.1016/j.icarus.2003.08.023

    View details for Web of Science ID 000221180400012

  • Heavy metal frost on Venus ICARUS Schaefer, L., Fegley, B. 2004; 168 (1): 215–19

    View details for DOI 10.1016/j.icarus.2003.11.023

    View details for Web of Science ID 000220161400020

https://orcid.org/0000-0003-2915-5025