Figures and Tables

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Introduction

Nitrogen is the most depleted element in the observable Earth when compared to CI chondrites, materials that most faithfully record the bulk composition of the solar system (observable Earth is the sum of the atmosphere, oceans, crust, and mantle) (e.g., Marty, 2012

Marty, B. (2012) The origins and concentrations of water, carbon, nitrogen and noble gases on earth. Earth and Planetary Science Letters 313–314, 56–66.

; Halliday, 2013

Halliday, A.N. (2013) The origins of volatiles in the terrestrial planets. Geochimica et Cosmochimica Acta 105, 146–171.

). The depletion of N is a fundamental expression of the integrated processes that determine the volatile budget of planets (Fig. 1).

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There are many early acting processes that can deplete nitrogen and other volatile elements, either in a bulk planet or its observable reservoirs. Chondrites have various volatile element patterns that may reflect formation in regions of the Solar System with fractionated volatiles or the operation of incomplete condensation/evaporation reactions (Bergin et al., 2015

Bergin, E.A., Blake, G.A., Ciesla, F., Hirschmann, M.M., Li, J. (2015) Tracing the ingredients for a habitable earth from interstellar space through planet formation. Proceedings of the National Academy of Sciences 112, 8965–8970.

). With accretion and differentiation, terrestrial bodies form atmospheres, and these atmospheres can be lost (Tucker and Mukhopadhyay, 2014

Tucker, J.M., Mukhopadhyay, S. (2014) Evidence for multiple magma ocean outgassing and atmospheric loss episodes from mantle noble gases. Earth and Planetary Science Letters 393, 254–265.

; Schlichting et al., 2015

Schlichting, H.E., Sari, R., Yalinewich, A. (2015) Atmospheric mass loss during planet formation: The importance of planetesimal impacts. Icarus 247, 81–94.

). Core formation occurs in parallel to planetary accretion, and because nitrogen can display both siderophile and lithophile behaviour, the effect of core formation on the apparent nitrogen depletion in Earth remains uncertain (Roskosz et al., 2013

Roskosz, M., Bouhifd, M.A., Jephcoat, A.P., Marty, B., Mysen, B.O. (2013) Nitrogen solubility in molten metal and silicate at high pressure and temperature. Geochimica et Cosmochimica Acta 121, 15–28.

; Kadik et al., 2015

Kadik, A., Koltashev, V., Kryukova, E., Plotnichenko, V., Tsekhonya, T., Kononkova, N. (2015) Solubility of nitrogen, carbon, and hydrogen in FeO–Na₂O–Al₂O₃–SiO₂ melt and liquid iron alloy: Influence of oxygen fugacity. Geochemistry International 53, 849–868.

; Li et al., 2016

Li, Y., Marty, B., Shcheka, S., Zimmermann, L., Keppler, H. (2016) Nitrogen isotope fractionation during terrestrial core-mantle separation. Geochemical Perspectives Letters 2, 138–147.

; Dalou et al., 2017

Dalou, C., Hirschmann, M.M., von der Handt, A., Mosenfelder, J., Armstrong, L.S. (2017) Nitrogen and carbon fractionation during core–mantle differentiation at shallow depth. Earth and Planetary Science Letters 458, 141–151.

; Grewal et al., 2019a

Grewal, D.S., Dasgupta, R., Holmes, A.K., Costin, G., Li, Y., Tsuno, K. (2019a) The fate of nitrogen during core-mantle separation on earth. Geochimica et Cosmochimica Acta 251, 87–115.

,b

Grewal, D.S., Dasgupta, R., Sun, C., Tsuno, K., Costin, G. (2019b) Delivery of carbon, nitrogen, and sulfur to the silicate earth by a giant impact. Science Advances 5, eaau3669.

; Speelmanns et al., 2019

Speelmanns, I.M., Schmidt, M.W., Liebske, C. (2019) The almost lithophile character of nitrogen during core formation. Earth and Planetary Science Letters 510, 186–197.

).

The role of pressure and temperature on core formation chemistry become larger for larger planetary bodies, as indicated by the refractory siderophile element concentrations observed for Earth, Mars, and Vesta (Righter and Drake, 1996

Righter, K., Drake, M.J. (1996) Core formation in Earth’s moon, Mars, and Vesta. Icarus 124, 513–529.

). Studies agree that increasing temperature makes nitrogen less siderophile (Grewal et al., 2019a

Grewal, D.S., Dasgupta, R., Holmes, A.K., Costin, G., Li, Y., Tsuno, K. (2019a) The fate of nitrogen during core-mantle separation on earth. Geochimica et Cosmochimica Acta 251, 87–115.

; Speelmanns et al., 2019

Speelmanns, I.M., Schmidt, M.W., Liebske, C. (2019) The almost lithophile character of nitrogen during core formation. Earth and Planetary Science Letters 510, 186–197.

). Extrapolating the temperature effect on metal-silicate partition coefficients for nitrogen (, atomic) to the average core formation temperature for Earth implies lithophile behaviour (e.g., Speelmanns et al., 2019

Speelmanns, I.M., Schmidt, M.W., Liebske, C. (2019) The almost lithophile character of nitrogen during core formation. Earth and Planetary Science Letters 510, 186–197.

). In the absence of a large effect of pressure, core formation would apparently have little ability to modify the observable budget of nitrogen during the accretion of larger rocky worlds, such as Earth.

Previously published high pressure experiments suggest that pressure favours N incorporation into cores (Roskosz et al., 2013

Roskosz, M., Bouhifd, M.A., Jephcoat, A.P., Marty, B., Mysen, B.O. (2013) Nitrogen solubility in molten metal and silicate at high pressure and temperature. Geochimica et Cosmochimica Acta 121, 15–28.

, Grewal et al., 2019a

Grewal, D.S., Dasgupta, R., Holmes, A.K., Costin, G., Li, Y., Tsuno, K. (2019a) The fate of nitrogen during core-mantle separation on earth. Geochimica et Cosmochimica Acta 251, 87–115.

); however, the pressure effect cannot be confidently resolved to be different from zero (Grewal et al., 2019a

Grewal, D.S., Dasgupta, R., Holmes, A.K., Costin, G., Li, Y., Tsuno, K. (2019a) The fate of nitrogen during core-mantle separation on earth. Geochimica et Cosmochimica Acta 251, 87–115.

). Towards this end, we report values from experiments conducted up to 26 GPa and 3437 K, using a laser heated diamond-anvil cell (LH-DAC). We supplement our LH-DAC data, with a systematic series of piston cylinder experiments to enable a robust parameterisation.

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Methods

We conducted lower P-T partitioning experiments (1773–2413 K, 0.95–2.38 GPa) using a piston cylinder (PC) and higher P-T experiments (3046–3437 K, 23.2–25.6 GPa) using a LH-DAC (Tables 1, S-1). Experimental fO₂ conditions ranged from ΔIW−6.6 to ΔIW−1.0 (log unit deviations from the iron-wüstite buffer). We quantified the composition of reacted metal-silicate pairs using field emission electron microprobe analysis (Table 1). An example backscatter image is provided in Figure S-1, along with a typical time-temperature path for LH-DAC experiments. We also compare major element partitioning data of LH-DAC experiments to literature data in Figure S-2 as an evaluation of data quality. Table S-2 reports starting materials compositions. Further details on methods are provided in the Supplementary Information.

Experiment	Note	Series	T, K	T, ±	P, GPa	P, ±	log(DN), atomic	log(γFe)	Ni, atomic	S, atomic	C, atomic	N, atomic	ΔIW
PC_N_EXP1		P, T, S, Ni, N, fO2, IP	1973	10	0.95	0.05	1.40	−0.08	0.000	0.000	0.159	0.024	−1.59
PC_N_EXP2	low S metal	S	1973	10	0.95	0.05	1.44	−0.06	0.000	0.014	0.133	0.038	−1.62
PC_N_EXP2	high S metal	S	1973	10	0.95	0.05	1.17	0.18	0.000	0.372	0.025	0.020	−1.80
PC_N_EXP3		fO2	1973	10	0.95	0.05	0.01	−0.01	0.000	0.000	0.053	0.002	−6.56
PC_N_EXP4		fO2	1973	10	0.95	0.05	−0.68	−0.04	0.000	0.000	0.109	0.003	−5.28
PC_N_EXP5		fO2	1973	10	0.95	0.05	−0.59	−0.06	0.000	0.000	0.136	0.007	−4.65
PC_N_EXP6		P	1973	10	2.38	0.05	1.36	−0.05	0.000	0.000	0.119	0.106	−1.61
PC_N_EXP7	high S metal	S	1973	10	2.38	0.05	1.43	−0.04	0.000	0.109	0.091	0.086	−1.57
PC_N_EXP8		fO2	1973	10	0.95	0.05	0.97	−0.07	0.000	0.000	0.142	0.031	−2.50
PC_N_EXP9		T	2373	10	1.05	0.05	0.77	−0.06	0.000	0.000	0.151	0.019	−1.64
PC_N_EXP10		T	2403	10	1.05	0.05	0.46	−0.07	0.000	0.000	0.160	0.013	−1.62
PC_N_EXP11	low S metal	S	2413	10	1.05	0.05	1.05	−0.06	0.000	0.012	0.143	0.033	−1.69
PC_N_EXP12	low S metal	S	1973	10	1.66	0.05	1.37	−0.05	0.000	0.030	0.111	0.074	−1.69
PC_N_EXP12	high S metal	S	1973	10	1.66	0.05	1.20	0.11	0.000	0.301	0.026	0.050	−1.78
PC_N_EXP13		Ni	1973	10	1.00	0.05	0.80	−0.05	0.225	0.000	0.117	0.019	−1.57
PC_N_EXP14		T, N	1773	10	0.95	0.05	1.56	−0.07	0.000	0.000	0.138	0.039	−1.70
PC_N_EXP15		Ni	1973	10	0.95	0.05	0.84	−0.07	0.012	0.000	0.143	0.032	−2.48
PC_N_EXP17		T, N	2173	10	1.05	0.05	0.90	−0.06	0.000	0.000	0.147	0.029	−1.64
PC_N_EXP18		T, N	1873	10	1.05	0.05	1.47	−0.07	0.000	0.000	0.146	0.033	−1.60
PC_N_EXP19		IP	1973	10	0.95	0.05	0.92	−0.08	0.000	0.000	0.157	0.030	−1.75
PC_N_EXP22		IP	1973	10	0.95	0.05	0.83	−0.06	0.000	0.000	0.137	0.042	−1.71
PC_N_EXP23		IP	1973	10	0.95	0.05	0.82	−0.07	0.000	0.000	0.149	0.036	−1.61
PC_N_EXP24		Ni	1973	10	0.95	0.05	1.11	−0.07	0.104	0.000	0.148	0.009	−1.85
DAC_N_EXP1 spot 2		P	3142	46	23.80	2.35	1.55	−0.06	0.256	0.000	0.160	0.135	−1.18
DAC_N_EXP1 spot 3		P	3437	255	25.60	3.90	1.78	−0.10	0.215	0.000	0.219	0.054	−0.96
DAC_N_EXP1 spot 4		P	3046	13	23.20	2.10	1.59	−0.06	0.303	0.000	0.154	0.118	−1.15

Series: P, pressure; T, temperature; S, sulfur; Ni, nickel; N-C, nitrogen-carbon; fO₂, oxygen fugacity; IP, ionic porosity; Ni, S, C, N, atomic fraction of metal phase.

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Results

We completed independent series of experiments to quantify the P-T-X controls on values (Fig. 2, Table 1). Individual series correlations indicate values depend strongly on fO₂ (R² = 0.99, p value = 0.005, n = 4), temperature (R² = 0.97, p value = 0.001, n = 6), and pressure (R² = 0.98, p value < 0.001, n = 9) over other conditions relevant to magma oceans (Fig. 2a,d), whereas , , , and the ionic porosity of silicate liquid have significant (p values < 0.05) but minor effects (Figs. 2b,c, S-4, S-5). Our fO₂ and temperature findings accord with previous work (Dalou et al., 2017

Dalou, C., Hirschmann, M.M., von der Handt, A., Mosenfelder, J., Armstrong, L.S. (2017) Nitrogen and carbon fractionation during core–mantle differentiation at shallow depth. Earth and Planetary Science Letters 458, 141–151.

; Grewal et al., 2019a

Grewal, D.S., Dasgupta, R., Holmes, A.K., Costin, G., Li, Y., Tsuno, K. (2019a) The fate of nitrogen during core-mantle separation on earth. Geochimica et Cosmochimica Acta 251, 87–115.

; Speelmanns et al., 2019

Speelmanns, I.M., Schmidt, M.W., Liebske, C. (2019) The almost lithophile character of nitrogen during core formation. Earth and Planetary Science Letters 510, 186–197.

). Our lower pressure experiments indicate that N-C interactions in Fe alloy make both elements less siderophile and yield an epsilon value () of 7.6 ± 1.4 (R² = 0.90, p value = 0.004, n = 6; Fig. S-4), qualitatively consistent with the Steelmaking Data Sourcebook (1988)

Steelmaking Data Sourcebook (1988) The Japan Society for the Promotion of Science: The 19th Committee on Steelmaking. Gordon and Breach Science Publishers, New York.

and values collected under C-free conditions (Grewal et al., 2021

Grewal, D.S., Dasgupta, R., Hough, T., Farnell, A. (2021) Rates of protoplanetary accretion and differentiation set nitrogen budget of rocky planets. Nature Geoscience 14, 369–376.

). Our value calculations follow the approach of Ma (2001)

Ma, Z. (2001) Thermodynamic description for concentrated metallic solutions using interaction parameters. Metallurgical and Materials Transactions B 32, 87–103.

.

Our LH-DAC experiments consistently demonstrated siderophile behaviour (Fig. 2d) despite their high temperature, and this requires a large, positive pressure effect. These high P-T experiments contain C and Ni, and were relatively oxidising. Quantifying the pressure effect therefore requires simultaneous consideration of these other parameters, which is enabled by our PC experiments (Equation 1, see below). Our determination of a positive effect of pressure is consistent with previous work, but the larger range of P we investigated results in more precise determination of the P-T coefficients in Equations 1 and 2 (c.f., Roskosz et al., 2013

Roskosz, M., Bouhifd, M.A., Jephcoat, A.P., Marty, B., Mysen, B.O. (2013) Nitrogen solubility in molten metal and silicate at high pressure and temperature. Geochimica et Cosmochimica Acta 121, 15–28.

, Grewal et al., 2019a

Grewal, D.S., Dasgupta, R., Holmes, A.K., Costin, G., Li, Y., Tsuno, K. (2019a) The fate of nitrogen during core-mantle separation on earth. Geochimica et Cosmochimica Acta 251, 87–115.

).

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To parameterise our data, we first recalculate experiments to a carbon-free baseline using our newly derived value. We then conduct an equal weight, least squares regression on parameters identified as significant in their individual series (1/T, P/T, , and ΔIW). Our approach yields the following expression (R² = 0.95, p value < 0.001, n = 22; Fig. 2e):

or if the effect of carbon is included in the parameterisation

Uncertainties are reported as 1σ. Note that , , and refer to the expanded concentration expression associated with the notation of Ma (2001)

Ma, Z. (2001) Thermodynamic description for concentrated metallic solutions using interaction parameters. Metallurgical and Materials Transactions B 32, 87–103.

, and that positive coefficients indicate a reduction in the value. Application of Equation 1 to a mantle liquidus geotherm at ΔIW−2 indicates a monotonic increase in with depth (Fig. 2f).

We parameterise our data alone because we completed systematic series of experiments to isolate specific effects on partitioning. Inclusion of all published data is accompanied by a large number of free parameters, and prevents resolution of N, S and C effects that are clearly observable in our results (Figs. 2, S-4). Predictions of Equation 1 are compared to literature data in Figures 2e, S-6. Additional details regarding this regression are provided in the Supplementary Information. The covariance matrix for Equation 1 is reported in Table S-3. We also report our fitting of literature data with the effects identified as significant here as Equation S-7.

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Modelling N Distribution throughout Earth

Having established that pressure strongly modulates values, we now calculate the equilibrium distribution of N and S between cores, magma oceans, and atmospheres for a range of plausible stratification conditions. We include S because multiple high pressure studies show agreement and now constrain its metal-silicate partitioning up to extreme P-T conditions. Our parameterisation of values is applied here and is detailed in the Supplementary Information (Fig. S-8).

Mass balance is used to solve for the equilibrium distribution of N and S as required by partitioning and magma solubility constraints (Equation 1; Libourel et al., 2003

Libourel, G., Marty, B., Humbert, F. (2003) Nitrogen solubility in basaltic melt. Part I. Effect of oxygen fugacity. Geochimica et Cosmochimica Acta 67, 4123–4135.

). The mantle is assumed to be completely molten, and the mass fraction of the core is 0.325. Uncertainties are evaluated by varying and according to their covariance matrices and iterating the mass balance model. No S is assumed to be present in the atmosphere given its relatively high solubility in magma. All scenarios assume a bulk planet S/N ratio set by enstatite chondrite (85) and that the magma ocean contains 225 ± 25 ppm S (Hirschmann, 2016

Hirschmann, M.M. (2016) Constraints on the early delivery and fractionation of Earth’s major volatiles from C/H, C/N, and C/S ratios. American Mineralogist 101, 540–553.

). We focus on enstatite chondrites because their average S/N ratio is intermediate between gas-rich (29; CI and CM) and ordinary chondrites (404; Wasson and Kallemeyn, 1988

Wasson, J.T., Kallemeyn, G.W. (1988) Compositions of chondrites. Philosophical Transactions of the Royal Society of London Series A, Mathematical and Physical Sciences 325, 535–544.

). Models that consider S/N ratios for other groups of chondrites are presented in the Supplementary Information (Figs. S-9, S-10).

Our first goal is to quantify how the S/N ratio of observable Earth (S/N_OE, 82 ± 29, dotted lines in Fig. 3a,c) varies in response to differentiation conditions. We consider models with core formation fO₂ of ΔIW−2 while varying core formation pressure and atmospheric fO₂ (Fig. 3). We focus on ΔIW−2 because the FeO content of Earth implies an average fO₂ for core formation near this value. Pressures of metal-silicate equilibration range up to 60 GPa, an upper limit in the single stage framework for Earth (e.g., Fischer et al., 2015

Fischer, R.A., Nakajima, Y., Campbell, A.J., Frost, D.J., Harries, D., Langenhorst, F., Miyajima, N., Pollok, K., Rubie, D.C. (2015) High pressure metal–silicate partitioning of Ni, Co, V, Cr, Si, and O. Geochimica et Cosmochimica Acta 167, 177–194.

). Our model takes a single stage approach, and while accretion is a multi-step process, single stage calculations capture average P-T-X conditions that can be readily compared between elements (Siebert et al., 2011

Siebert, J., Corgne, A., Ryerson, F.J. (2011) Systematics of metal–silicate partitioning for many siderophile elements applied to earth’s core formation. Geochimica et Cosmochimica Acta 75, 1451–1489.

). Atmospheric fO₂ varies in our model between ΔIW−3 and ΔIW+3. Atmospheric fO₂ conditions are a free parameter in light of evidence for the depth dependence of the Fe⁺³/Fe_tot ratio of magma in equilibrium with iron (Zhang et al., 2017

Zhang, H., Hirschmann, M., Cottrell, E., Withers, A. (2017) Effect of pressure on Fe³⁺/Fe ratio in a mafic magma and consequences for magma ocean redox gradients. Geochimica et Cosmochimica Acta 204, 83–103.

; Armstrong et al., 2019

Armstrong, K., Frost, D.J., McCammon, C.A., Rubie, D.C., Ballaran, T.B. (2019) Deep magma ocean formation set the oxidation state of earth’s mantle. Science 365, 903–906.

; Deng etal., 2020

Deng, J., Du, Z., Karki, B., Ghosh D., Lee, K. (2020) A magma ocean origin to divergent redox evolutions of rocky planetary bodies and early atmospheres. Nature Communications 11, 2007.

) and the temperature dependence of Fe⁺³/Fe_tot for any fO₂ (Sossi et al., 2020

Sossi, P.A., Burnham, A.D., Badro, J., Lanzirotti, A., Newville, M., O’Neill, H.S.C. (2020) Redox state of earth’s magma ocean and its venus-like early atmosphere. Science Advances 6, eabd1387.

).

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Our models demonstrate the strong sensitivity of S/N_OE ratios to core formation pressure; at low pressure (<10 GPa), S/N_OR ratios are low, but with increasing pressure, S/N_OE ratios rise as S becomes less siderophile and N becomes more siderophile. The rise is such that core formation near 30 GPa results in S/N_OE ratios that match Earth for more reducing atmospheres. More oxidising atmospheres require higher pressure core formation to satisfy Earth’s S/N_OE ratio, as more N remains in the atmosphere, unable to partition into the core (Fig. 3a,b).

It is possible that the atmosphere is partially lost during accretion, leading to preferential depletion of N relative to S. We model this possibility as the end member of the magma ocean being the only contributor of N and S to later-forming observable reservoirs (Fig. 3c,d). In these cases S/N_OE,MO (S/N ratio of the magma ocean) also matches Earth near 30 GPa, and model results are relatively insensitive to atmospheric fO₂. Cases of intermediate atmospheric loss plot between the two end members for atmospheric contribution considered here (c.f., Fig. 3a–d).

Taken together, our models demonstrate that higher pressure core formation scenarios can satisfy the S/N_OE ratio of Earth, assuming a bulk planet S/N ratio similar to enstatite chondrite. Bulk planet S/N ratios closer to gas-rich chondrites (low S/N) require even higher core formation pressures, while bulk planet S/N ratios closer to ordinary chondrites (high S/N) require lower pressure to satisfy the S/N_OE ratio constraint (Figs. S-9, S-10). This all serves to highlight the importance of core formation pressure for modulating planetary volatile budgets.

It is significant that higher pressure core formation (>30 GPa) and a core-mantle fO₂ of ΔIW−2 can produce S/N_OE ratios equal to Earth because these are the same differentiation conditions implied by moderately siderophile element and FeO concentrations in the observable Earth in a single stage framework (e.g., Siebert et al., 2011

Siebert, J., Corgne, A., Ryerson, F.J. (2011) Systematics of metal–silicate partitioning for many siderophile elements applied to earth’s core formation. Geochimica et Cosmochimica Acta 75, 1451–1489.

; Fischer et al., 2015

Fischer, R.A., Nakajima, Y., Campbell, A.J., Frost, D.J., Harries, D., Langenhorst, F., Miyajima, N., Pollok, K., Rubie, D.C. (2015) High pressure metal–silicate partitioning of Ni, Co, V, Cr, Si, and O. Geochimica et Cosmochimica Acta 167, 177–194.

). Importantly, higher pressure core formation also yields a bulk planet with 6650–2050 ppm S (30–60 GPa) (Fig. 3e), and these values compare favourably with estimates of 5600 ppm S for bulk Earth based on the volatility trend (Dreibus and Palme, 1996

Dreibus, G., Palme, H. (1996) Cosmochemical constraints on the sulfur content in the Earth’s core. Geochimica et Cosmochimica Acta 60, 1125–1130.

). The multiple successes of higher pressure models for explaining Earth’s volatile budget are important because they suggest that volatiles are modulated by the same core formation events that modulate refractory elements. This suggestion contrasts with previous hypotheses that smaller, volatile-rich bodies preferentially contributed to Earth’s volatile budget (e.g., Grewal et al., 2019b

Grewal, D.S., Dasgupta, R., Sun, C., Tsuno, K., Costin, G. (2019b) Delivery of carbon, nitrogen, and sulfur to the silicate earth by a giant impact. Science Advances 5, eaau3669.

), decoupling the accretion of life-enabling elements from refractory elements.

It is well established within the Solar System that planetary body size correlates with average core formation pressures (Righter and Drake, 1996

Righter, K., Drake, M.J. (1996) Core formation in Earth’s moon, Mars, and Vesta. Icarus 124, 513–529.

), and our work therefore predicts a direct relationship between planet size and its distribution of volatiles. This link should enable more precise evaluations of exoplanet habitability, worlds for which size remains a central constraint on their geologic evolution.

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Acknowledgements

We acknowledge discussions with Ian Ocampo during a summer internship at NMNH. We additionally acknowledge the support provided by C. Prescher, E. Greenberg, and V. Prakapenka during the experiments conducted at GSECARS and in data reduction. We thank Rob Wardell and Tim Rose for their support of the microscopy work associated with this manuscript. We thank Tim McCoy for discussions regarding the model results.

CRMJ acknowledges support by NSF-EAR grant 1725315, NASA grant 80NSSC21K0377, Smithsonian GVP fellowship, Carnegie Institution for Science (Geophysical Lab) Fellowship, and start up from Tulane University. Experiments were partially supported by NASA grant to YF. ZD thanks the support from Carnegie Fellowship, grants from Chinese Academy of Sciences and State Key Laboratory of Isotope Geochemistry (No. 29Y93301701, 51Y8340107), as well as Strategic Priority Research Program (B) (XDB18030604). Portions of this work were performed at GeoSoilEnviroCARS (The University of Chicago, Sector 13), the Advanced Photon Source, Argonne National Laboratory. GeoSoilEnviroCARS is supported by the National Science Foundation–Earth Sciences (EAR 1128799) and the Department of Energy–GeoSciences (DE-FG02-94ER14466). This research used resources of the Advanced Photon Source, a US Department of Energy (DOE) Office of Science User Facility operated for the DOE Office of Science by Argonne National Laboratory under contract number DE-AC02-06CH11357.

Editor: Cin-Ty Lee

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References

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Supplementary Information

The Supplementary Information includes:

• Experimental Methods
• Demonstrations of Equilibrium
• Validation of Predictive Power of Equations 1 and 2
• Further Details for Nitrogen Distribution Model
• Model Results for Other Chondrite Groups
• Tables S-1 to S-3
• Figures S-1 to S-10
• Supplementary Information References

Download Tables S-1 to S-3 (Excel).

Download the Supplementary Information (PDF).