About

Richard Hervig is a Professor in the School of Earth and Space Exploration at Arizona State University. He earned his B.S. degree from the University of Iowa in 1975 and his Ph.D. from the University of Chicago in 1979. Following his doctoral studies, Hervig spent a year conducting research on nuclear waste disposal at the Hanford Nuclear Reservation in Washington State. He then joined Arizona State University as a postdoctoral researcher working with Alex Navrotsky, focusing on the thermodynamic properties of various silicate glasses. Subsequently, he transitioned to a research position in Peter Williams' secondary ion mass spectrometry (SIMS) laboratory, where he applied SIMS techniques to address problems in geochemistry and cosmochemistry. Hervig was promoted to full professor in 2004 within the Department of Geology, which is now part of the School of Earth and Space Exploration.

Research topics

• Geochemistry
• Geology
• Chemistry
• Astrobiology
• Physics
• Optics
• Nuclear physics
• Materials science
• Mineralogy
• Astrophysics
• Thermodynamics

Selected publications

• The Extent of Solar Energetic Particle Irradiation in the Sun’s Protoplanetary Disk

  The Astrophysical Journal · 2026-01-23

  articleOpen access

  Abstract Solar flares emit X-rays and high-energy (MeV to GeV) ions called solar energetic particles (SEPs). Astronomical observations show solar-mass protostellar fluxes are a factor Φ ≈ 3 × 10 2 –3 × 10 3 times higher than the present-day Sun. Constraining Φ in the early solar system is important for modeling ionization in the Sun’s protoplanetary disk, the extent of magnetorotational instability or magnetocentrifugal outflows, or even production of short-lived radionuclides. Recent interpretations of meteoritic data—including cosmogenic Ne in hibonite grains, initial <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mo stretchy="false">(</mml:mo> <mml:msup> <mml:mrow> <mml:mspace width="0.25em"/> </mml:mrow> <mml:mrow> <mml:mn>10</mml:mn> </mml:mrow> </mml:msup> <mml:mi mathvariant="normal">Be</mml:mi> <mml:mo>/</mml:mo> <mml:msup> <mml:mrow> <mml:mspace width="0.25em"/> </mml:mrow> <mml:mrow> <mml:mn>9</mml:mn> </mml:mrow> </mml:msup> <mml:mi mathvariant="normal">Be</mml:mi> <mml:mo stretchy="false">)</mml:mo> </mml:mrow> <mml:mrow> <mml:mn>0</mml:mn> </mml:mrow> </mml:msub> </mml:math> ratios in Ca-rich, Al-rich inclusions (CAIs), or even inferences of live 7 Be in CAIs—suggest values Φ &gt; 10 5 , reaching as high as Φ ≈ 6 × 10 6 , which would make the young Sun extraordinarily active, even for a protostar. We constrain Φ by reexamining these data. We conclude that cosmogenic Ne was produced in hibonite grains as they resided in the disk; 36 Cl was created in Cl-poor grains after the disk dissipated; 10 Be was inherited from the molecular cloud, with almost no (&lt;1%) 10 Be created in the disk; and there is no evidence whatsoever for any live 7 Be in CAIs. We show these data are consistent with a value Φ ≈ 3 × 10 3 for the first &gt;5 Myr of the solar nebula. The early Sun evidently emitted a flux of X-rays and SEPs not atypical for a protostar.

  PublisherDOI

• Trace Element Analyses of Plagioclase from Troctolite 76535 and Implications for Mg-suite Petrogenesis

  2025-01-21

  preprint

  Certain Mg-suite samples display enrichment in incompatible elements, likely resulting from the assimilation of the material that crystallized at the very late stages of magma ocean (ur-KREEP). This study uses trace element analyses of plagioclase separates from sample 76535 to estimate the Rare Earth Element (REE) concentration of the Mg-suite parental liquid and assess the extent of contribution from ur-KREEP. Thirty-three trace elements, including REEs, were measured in the separates and the measured REEs reflect magmatic conditions being free from subsolidus alteration. The Mg-suite parental liquid was estimated using these REE data as targets for a Python-based forward model which employs a RhyoliteMELTS-defined liquid line of descent. The estimated parental liquid shows REE enrichments of 200 times chondritic levels for Light REEs and 20 times for Heavy REEs. Mixing models between the REE compositions of a potential Mg-suite primary liquid and modeled ur-KREEP indicate that 30-50% assimilation of ur-KREEP is required to reproduce the observed REE concentrations in the Mg-suite parental liquid. We demonstrate an approach to determine the petrogenesis of a sample by characterizing a very limited quantity of grains, in an effort to maximize the scientific output from current and future returned samples such as Artemis.

  PublisherDOI

• Evidence of Double-Medium Diffusion in Trace Element Depth Profiles of Human and Mammoth Enamel

  2025-01-01

  articleSenior author
  PublisherDOI

• Trace element analyses of plagioclase from troctolite 76535 and implications for the petrogenesis of the lunar highlands Mg‐suite

  Meteoritics and Planetary Science · 2025-09-09

  article

  Abstract We used trace element analyses of plagioclase from Mg‐suite troctolite 76535 to estimate the Rare Earth Element (REE) concentrations of its parental liquid and assess the feasibility of an urKREEP contribution to the Mg‐suite parental liquid. We measured 33 trace elements in 76535 plagioclase separates. Our measurements revealed enrichments in incompatible elements consistent with previous analyses. Using the measured REE concentrations, we estimated the REE concentrations of the unfractionated Mg‐suite parental liquid using a RhyoliteMELTS‐based forward model. Compared to chondritic concentrations, the Mg‐suite parental liquid is ~100 times more enriched in light REEs and ~10 times more enriched in heavy REEs. We sought to explore the feasibility of reproducing these enrichments in the parental liquid through assimilation of urKREEP by a partial melt of rising LMO cumulates during cumulate mantle overturn. We show that these enrichments can be reproduced by a 30%–50% addition of fully molten urKREEP to the LMO cumulate melt, if the LMO cumulate melt and urKREEP are in thermal equilibrium with each other. However, the Mg# of these mixtures (57–68) is too low to produce the most Mg‐rich olivine (Fo 91) observed in Mg‐suite troctolites. Alternatively, assuming that the LMO cumulate melt and urKREEP are in thermal disequilibrium, we reproduced both the REE abundances and Mg# of the Mg‐suite parental liquid with only a 10% addition of the urKREEP partial melt. These results support the feasibility of urKREEP assimilation as a mechanism for generating the incompatible element enrichments in Mg‐suite magmas while preserving their major element chemistry.

  PublisherDOI

• “Canode”: A conical partially magnetic anode for efficient negative ion extraction from duoplasmatron ion sources

  Journal of Vacuum Science & Technology B Nanotechnology and Microelectronics Materials Processing Measurement and Phenomena · 2025-06-24

  article

  We report on the design and performance of an improved duoplasmatron ion source for secondary ion mass spectrometers. The source is designed specifically to optimize extraction of negative oxygen ions while suppressing electron extraction using a built-in magnetic asymmetry in the anode electrode. Other changes from conventional designs are (a) drilling the ion extraction aperture directly into the magnetic steel anode rather than in a refractory (nonmagnetic) metal insert, thereby eliminating a magnetic “hole” that acts to counter the desired magnetic concentration of the discharge at the aperture and (b) forming the anode into a conical shape convex toward the intermediate electrode to increase the magnetic field concentration at the extraction aperture, hence the term “Canode.” The built-in magnetic asymmetry allows the width and shape of the intermediate electrode to be varied to further optimize magnetic concentration of the discharge. Tests were performed with both ims 6f and NanoSIMS 50L instruments manufactured by Cameca Instruments, Inc. (Fitchburg, WI, USA). In the ims 6f, the Canode design gave O− primary ion currents up to a factor of five greater than the factory ion source design. In the NanoSIMS 50L, the Canode source produced a focused O− ion beam at the sample with a diameter of 50 nm, identical to the performance of the radio-frequency Hyperion ion source developed by Oregon Physics (Beaverton, OR, USA) and offered as an option by Cameca.

  PublisherDOI

• New Constraints on Trace Element Diffusion Rates in Tooth Enamel Bioapatite

  Abstracts with programs - Geological Society of America · 2025-01-01

  articleSenior author
  PublisherDOI

• Effects of Crystal Orientation and Temperature on Space Irradiation of Silicates

  The Astrophysical Journal · 2025-09-25

  articleOpen access

  Abstract Space irradiation plays a crucial role in surface weathering and hydration processes of airless bodies in the solar system. Despite extensive laboratory studies, the impact of crystal orientation and temperature on these irradiation processes remains poorly understood. In this study, we conducted hydrogen-implantation experiments on olivine crystals, controlling both crystal orientation and temperature. Our results reveal that the amount and depth of implanted hydrogen depend on the crystal orientation. Olivine exhibits the largest resistance to ion irradiation along the [100] direction, resulting in a thinner damaged region (∼180–200 nm) and subsurface vesicle formation. In contrast, the [010] and [001] orientations allow deeper damage (∼200–210 nm) accompanied by fracturing. Additionally, increasing temperatures from 25°C to 200°C promote the saturation and retention of implanted hydrogen. However, above a critical temperature (∼200°C for olivine), hydrogen levels stabilize, and no further increase is observed. These findings highlight the critical role of crystal orientation and temperature in the irradiation process, providing important constraints for numerical models simulating the effects of space irradiation on rocky bodies.

  PublisherDOI

• The Extent of Solar Energetic Particle Irradiation in the Sun's Protoplanetary Disk

  ArXiv.org · 2025-12-02

  preprintOpen access

  Solar flares emit X rays and high-energy (MeV-GeV) ions (Solar Energetic Particles, or SEPs). Astronomical observations show solar mass-protostellar fluxes are a factor $Φ\approx 3 \times 10^2 - 3 \times 10^3$ times higher than the present-day Sun. Constraining $Φ$ in the early solar system is important for modeling ionization in the Sun's protoplanetary disk, the extent of magnetorotational instability or magnetocentrifugal outflows, or even production of short-lived radionuclides. Recent interpretations of meteoritic data -- cosmogenic Ne in hibonite grains, initial $({}^{10}{\rm Be}/{}^{9}{\rm Be})_0$ ratios in Ca-rich, Al-rich inclusions (CAIs), or even inferences of live ${}^{7}{\rm Be}$ in CAIs -- have suggested values $Φ&gt; 10^5$, even as large as $Φ\approx 6 \times 10^6$, which would make the young Sun extraordinarily active, even for a protostar. We constrain $Φ$ by re-examining these data. We conclude: cosmogenic Ne was produced in hibonite grains as they resided in the disk; ${}^{36}{\rm Cl}$ was created in Cl-poor grains after the disk dissipated; ${}^{10}{\rm Be}$ was inherited from the molecular cloud, with almost no ($&lt; 1\%$) ${}^{10}{\rm Be}$ created in the disk; and there is no evidence whatsoever for any live ${}^{7}{\rm Be}$ in CAIs. We show these data are consistent with a value $Φ\approx 3 \times 10^3$ for the first $&gt; 5$ Myr of the solar nebula. The early Sun evidently emitted a flux of X rays and SEPs not atypical for a protostar.

  PublisherOA PDFDOI

• How Hot is the Moon: Quantifying the Role of Heat-Producing Elements on the Present-Day Selenotherm with Partitioning Experiments and Conductive Thermal Modeling

  2024-06-04 · 1 citations

  preprintOpen access

  Points• Reasonable present-day selenotherms produced by bulk U and Th abundances from dominantly enstatitic meteorites rather than carbonaceous chondrites • Mantle overturn and sinking of heat-producing-element-enriched high Fe-Ti cumulates associated with magma ocean crystallization was inefficient • Heat-producing element enriched high Fe-Ti cumulates are potentially present below the crust and fueled prolonged lunar volcanism

  PublisherOA PDFDOI

• HOW HOT IS THE MOON? A PERSPECTIVE FROM HEAT-PRODUCING ELEMENTS ON THE PRESENT-DAY SELENOTHERM THROUGH PARTITIONING EXPERIMENTS AND CONDUCTIVE THERMAL MODELING

  Abstracts with programs - Geological Society of America · 2024-01-01

  article
  PublisherDOI

Recent grants

• Community Facility Support: The Arizona State University SIMS Laboratories

  NSF · $1.6M · 2018–2026

• Facility Support: The Arizona State University SIMS Laboratories

  NSF · $970k · 2010–2015

• Facility Support: The Arizona State University Secondary Ion Mass Spectrometer (SIMS) Laboratories

  NSF · $710k · 2007–2011

• Facility Support: The Arizona State University SIMS Laboratories

  NSF · $1.2M · 2015–2019

• MARGINS Post-doctoral fellowship - Jeremy Boyce: Exploring the Record of Magmatic Volatiles in a Volcanic Arc via H, C, F, S, and Cl in Apatite

  NSF · $208k · 2006–2009

Frequent coauthors

• M. Wadhwa

  Arizona State University

  27 shared

• Lynda B. Williams

  Arizona State University

  26 shared

• A. J. G. Jurewicz

  Dartmouth College

  21 shared

• K. D. Rieck

  New Mexico Consortium

  21 shared

• J. V. Smith

  18 shared

• David R. Bell

  Scotland's Rural College

  14 shared

• Paul Bremner

  13 shared

• J. B. Lowenstern

  12 shared

Education

• Ph.D.

  University of Chicago

  1979

• B.S.

  University of Iowa

  1975