1) Olivine phenocrysts from basalts in several locations have higher nickel contents than expected from normal mantle peridotite sources, indicating a nickel-rich source.
2) Modeling of crystallization processes shows these olivines require a source with around 20% more nickel (2,360 ppm) than estimated for normal fertile peridotite (1,960 ppm).
3) The nickel-rich source is proposed to have formed from interaction of the core and mantle during crystallization of a basal magma ocean or melt-rich layer, and continues to be sampled by mantle plumes, such as those producing the basalts studied.
Controls on the fo and ni contents of olivine in sulfide bearing mafic ultram...xirey
This document summarizes controls on the nickel and magnesium contents of olivine in mafic and ultramafic intrusions. It discusses how fractional crystallization, reaction with sulfide liquids, and trapped liquid modification can impact olivine composition. It then uses examples from the Voisey's Bay intrusion in Canada, which hosts a major nickel-copper deposit, to demonstrate modeling approaches to understand these processes and better interpret olivine compositions in such intrusions.
A massive pulsar_in_a_compact_relativistic_binarySérgio Sacani
1) Researchers observed the pulsar PSR J0348+0432 in a compact orbit with a white dwarf companion. Timing observations yielded component masses - the pulsar has a precisely determined mass of 2.01 solar masses, among the highest yet observed.
2) Optical spectroscopy of the white dwarf companion found it has a mass of 0.172 solar masses. Analysis of the orbital parameters and component masses showed the system's orbital decay matches predictions from general relativity.
3) The high pulsar mass and compact orbit make this a sensitive laboratory for testing strong-field gravity. The observed orbital decay is consistent with general relativity, supporting its validity even in extreme gravity regimes not previously tested. This has implications
1. The spectrum of the bright Kuiper Belt object 2005 FY9 is dominated by methane absorption features in the near-infrared region. However, the methane absorption lines are significantly broader than seen on any other solar system body, indicating unusually long optical path lengths through methane grains on 2005 FY9, estimated to be around 1 cm in size.
2. In addition to methane, the spectrum also shows clear evidence for ethane, which is expected to form from UV photolysis of methane. No evidence is found for nitrogen or carbon monoxide, both known to be present on Pluto.
3. The differences between 2005 FY9's spectrum and those of Pluto and 2003 UB313 are suggested
This document appears to be a citation to a conference paper from 1981 that does not provide any other contextual information. As such, it is not possible to generate a meaningful summary with only this citation provided. Additional context and details would be needed to understand the topic and main points discussed in the referenced conference paper in order to write an informative summary.
An earth mass_planet_orbiting_alpha_centauri_bSérgio Sacani
1) Researchers have detected the smallest minimum mass planet found to date orbiting a solar-type star, Alpha Centauri B.
2) The planet has a minimum mass similar to Earth and orbits Alpha Centauri B with a period of 3.236 days, making it the closest exoplanet to our solar system discovered so far.
3) The detection demonstrates the ability to reach precision needed to detect potentially habitable super-Earth planets around Sun-like stars using radial velocity techniques, though this planet is too close to its star to be habitable.
The effects of_the_target_material_properties_and layering_on_the_crater_chro...Sérgio Sacani
This document summarizes a study analyzing the effects of target material properties and layering on determining crater ages for the Raditladi and Rachmaninoff basins on Mercury. The authors derive model ages of about 3.6 billion years for Rachmaninoff basin and 1.1 billion years for Raditladi basin. They also constrain the age of smooth plains within the basin floors, suggesting volcanic activity on Mercury may have continued until around 1 billion years ago or less. The study addresses the importance of considering terrain parameters such as mechanical properties and layering in the age determination process.
This document discusses observations of the Carina region made by the AGILE gamma-ray satellite over 130 days between 2007 and 2009. It detected a gamma-ray source, 1AGL J1043-5931, that is consistent with the position of Eta Carinae. Notably, 1AGL J1043-5931 exhibited a two-day gamma-ray flaring episode in October 2008. If associated with the Eta Car system, this would provide the first detection above 100 MeV of gamma rays from a colliding wind binary star system. The Carina region contains many massive stars, clusters, nebulae and a giant molecular cloud, making it complex to study.
Controls on the fo and ni contents of olivine in sulfide bearing mafic ultram...xirey
This document summarizes controls on the nickel and magnesium contents of olivine in mafic and ultramafic intrusions. It discusses how fractional crystallization, reaction with sulfide liquids, and trapped liquid modification can impact olivine composition. It then uses examples from the Voisey's Bay intrusion in Canada, which hosts a major nickel-copper deposit, to demonstrate modeling approaches to understand these processes and better interpret olivine compositions in such intrusions.
A massive pulsar_in_a_compact_relativistic_binarySérgio Sacani
1) Researchers observed the pulsar PSR J0348+0432 in a compact orbit with a white dwarf companion. Timing observations yielded component masses - the pulsar has a precisely determined mass of 2.01 solar masses, among the highest yet observed.
2) Optical spectroscopy of the white dwarf companion found it has a mass of 0.172 solar masses. Analysis of the orbital parameters and component masses showed the system's orbital decay matches predictions from general relativity.
3) The high pulsar mass and compact orbit make this a sensitive laboratory for testing strong-field gravity. The observed orbital decay is consistent with general relativity, supporting its validity even in extreme gravity regimes not previously tested. This has implications
1. The spectrum of the bright Kuiper Belt object 2005 FY9 is dominated by methane absorption features in the near-infrared region. However, the methane absorption lines are significantly broader than seen on any other solar system body, indicating unusually long optical path lengths through methane grains on 2005 FY9, estimated to be around 1 cm in size.
2. In addition to methane, the spectrum also shows clear evidence for ethane, which is expected to form from UV photolysis of methane. No evidence is found for nitrogen or carbon monoxide, both known to be present on Pluto.
3. The differences between 2005 FY9's spectrum and those of Pluto and 2003 UB313 are suggested
This document appears to be a citation to a conference paper from 1981 that does not provide any other contextual information. As such, it is not possible to generate a meaningful summary with only this citation provided. Additional context and details would be needed to understand the topic and main points discussed in the referenced conference paper in order to write an informative summary.
An earth mass_planet_orbiting_alpha_centauri_bSérgio Sacani
1) Researchers have detected the smallest minimum mass planet found to date orbiting a solar-type star, Alpha Centauri B.
2) The planet has a minimum mass similar to Earth and orbits Alpha Centauri B with a period of 3.236 days, making it the closest exoplanet to our solar system discovered so far.
3) The detection demonstrates the ability to reach precision needed to detect potentially habitable super-Earth planets around Sun-like stars using radial velocity techniques, though this planet is too close to its star to be habitable.
The effects of_the_target_material_properties_and layering_on_the_crater_chro...Sérgio Sacani
This document summarizes a study analyzing the effects of target material properties and layering on determining crater ages for the Raditladi and Rachmaninoff basins on Mercury. The authors derive model ages of about 3.6 billion years for Rachmaninoff basin and 1.1 billion years for Raditladi basin. They also constrain the age of smooth plains within the basin floors, suggesting volcanic activity on Mercury may have continued until around 1 billion years ago or less. The study addresses the importance of considering terrain parameters such as mechanical properties and layering in the age determination process.
This document discusses observations of the Carina region made by the AGILE gamma-ray satellite over 130 days between 2007 and 2009. It detected a gamma-ray source, 1AGL J1043-5931, that is consistent with the position of Eta Carinae. Notably, 1AGL J1043-5931 exhibited a two-day gamma-ray flaring episode in October 2008. If associated with the Eta Car system, this would provide the first detection above 100 MeV of gamma rays from a colliding wind binary star system. The Carina region contains many massive stars, clusters, nebulae and a giant molecular cloud, making it complex to study.
Role of trace elements in rare earth elementsPramoda Raj
Trace elements play an important role in igneous petrogenesis and can be used to understand magmatic processes. Trace elements are classified based on their behavior into incompatible and compatible elements. Rare earth elements (REE) are especially useful as their near-parallel patterns can indicate crystal fractionation. REE and other trace element analyses help determine the source depth of primary magmas and identify fractionating phases. Trace element discrimination diagrams also allow determination of paleotectonic settings. Overall, trace element studies provide insights into magma differentiation, source characterization, and petrogenetic modeling.
At the 2010 Prospector's and Developers Association of Canada (PDAC) Conference, David Lentz and Anthony Mariano gave a presentation on ranking and evaluating light to heavy rare earth deposits worldwide. This is that presentation.
Commerce Resources Corp. reports the results of a prospecting and sampling program completed on the Eldor Property. The results of this program are extremely encouraging, including the highest niobium mineralized sample collected to date from the area: 5.9% Nb2O5.
Role of Trace Elements In Petrogenesis Gokul Anand
Trace elements occur in very low concentrations in rocks and provide important information about magmatic processes. They can be classified as compatible or incompatible based on whether they fit easily into mantle mineral crystal structures. Geochemical analysis of trace elements using techniques like XRF and ICP-MS allows determination of magma source and depth, identification of fractionating phases, and testing of models of magmatic differentiation. Trace elements are especially useful for rare earth elements, which indicate the type of basalt and can identify fractionating phases from REE patterns.
The document provides an overview of mining potential and opportunities in the Philippines. It discusses the country's long history of mining dating back to the 16th century and rich diversity of metallic and non-metallic mineral resources. It highlights several major recent porphyry copper-gold discoveries, including the Far Southeast and Boyongan deposits. The minerals sector provides significant economic contributions and employment. Many areas remain underexplored and offer potential for further discoveries of copper, gold, and other mineral deposits.
The document summarizes the results of serpentinization of ultramafic rocks. There are three main products depending on the original rock composition: serpentinite and brucite from the serpentinization of dunites; serpentinite from the serpentinization of peridotites; and serpentinite and talc from the serpentinization of pyroxenites. Field studies in Guatemala identified dunite, lherzolite, and pyroxenite samples. Petrographic analysis found the rocks contain nickel-bearing minerals formed during serpentinization, including awaruite, pentlandite, and nickel-bearing serpentine and magnetite.
Nesosilicates or orthosilicates, have the orthosilicate ion, which constitute isolated (insular) [SiO4]4- tetrahedra that are connected only by interstitial cations. The atomic packing of the nesosilicate structure is generally dense which causes the mineral of this group to have relatively high specific gravity and hardness. The crystal habit of thee mineral is generally equidimensional and they have poor cleavage. The simplest structure in nesosilicates have mineral forsterite Mg2[SiO4]. These properties also that nesosilicates incorporate a considerable number of gemstones.
This document provides information about the mineral olivine. It begins with an introduction to olivine, noting its color and importance as a rock-forming mineral. It then discusses the members of the olivine family, their weathering, solid solution behavior, and position in Bowen's reaction series. The remainder of the document covers olivine's structure, alteration, high-pressure polymorphs, physical and optical properties, paragenesis, significance, and examples of occurrences. Diagrams and images supplement the detailed information presented.
This document provides background information on the Kalahari Craton in southern Africa, which consists of the Archaean Zimbabwe and Kaapvaal Cratons separated by the Limpopo Mobile Belt. It discusses the geological history and tectonic setting of the craton and its constituent terranes. The focus is on peridotite xenoliths from the Letlhakane kimberlite mine in northern Botswana, which will be studied to characterize the sub-cratonic lithospheric mantle beneath this region and better understand its origin and modification over time. A variety of analytical techniques will be used, including petrography, geochemistry, and Sm-Nd and Lu-Hf isotope analyses
This document provides an overview of talc mineralization in Nigeria. It discusses the geology of Nigeria and the formation of talc deposits. Talc deposits are found within Nigeria's schist belts in varied geologic and petrographic forms. Case studies of talc occurrences in locations like Wonu, Iseyin, Ilesha, and Isanlu are provided with details on the mineralization and rock associations at each site. The document concludes that talc deposits in Nigeria show marked variability in mineralization and petrographic properties.
[American mineralogist] a terrestrial magmatic hibonite grossite-vanadium ass...James AH Campbell
[American mineralogist] a terrestrial magmatic hibonite grossite-vanadium assemblage desilication and extreme reduction in a volcanic plumbing system mount carmel israel
A terrestrial magmatic hibonite grossite-vanadium assemblage desilication an...James AH Campbell
This document summarizes a study of a unique terrestrial occurrence of magmatic hibonite and grossite assemblages found in ejecta from Cretaceous pyroclastic deposits on Mount Carmel, Israel. The assemblages formed from calcium-aluminum rich silicate melts under extremely reducing conditions comparable to meteoritic counterparts. Textural evidence indicates hibonite first crystallized late after corundum and other phases, followed by grossite and spinel. Native vanadium spheres are included within hibonite, grossite and spinel, representing the most reduced conditions. Ongoing studies suggest the reducing conditions reflect interaction between basaltic magmas and mantle-derived methane-hydrogen fluids, resulting in
Highest niobium mineralized sample to date at MirannaStephan Bogner
Last week, the company reported sampling assays from the Miranna Area, located only 1 km east of its Ashram REE Deposit in Québec. The best results include 5.9% and 4.2% niobium pentoxide (Nb2O5). The 9 selected samples reported by Commerce averaged 2.3% Nb2O5. Of all 64 samples, 40 assayed >0.5% Nb2O5, with 16 surpassing 1%. Sampling also found significant grades of tantalum, phosphate and rare earth oxides (2 samples each graded >1,000 ppm Ta2O5 and 1% Nb2O5, while several samples revealed >10% P2O5).
When comparing these niobium grades with the range of global average mining grades of about 0.5 to 1.5% Nb2O5, and the average grades of niobium exploration projects, Commerce Resources indeed has every reason for being enthusiastic.
Niobium focused juniors seem to be enjoying a recent lift in share prices and market valuations potentially due to positive demand growth for niobium for structural steel for infrastructure projects, as well as for the current lighter and stronger chassis for cars. MDN Inc. has recently seen its’ share price appreciate by almost 400% following the announcement of their acquisition of the James Bay Niobium Project, called the Argor Project, which has an historic indicated resource with a grade of 0.52% Nb2O5.
Last year, NioCorp Developments Ltd. (originally structured by Zimtu Capital Corp.) reported an average indicated resource grade of 0.71% Nb2O5 assuming a 0.3% cut-off grade at its Elk Creek Niobium Deposit in Nebraska, USA. Today, NioCorp enjoys a market valuation exceeding $150 million CAD.
The document summarizes a study of the Groote Eylandt manganese orebody in Australia. The objectives of the study were to construct an accurate resource/reserve model using over 5,500 drill holes to satisfy reporting standards. Previous models were outdated and inaccurate. Key challenges included the orebody's variability and complex geological history. The new model incorporated stratigraphic units, addressed issues like downhole smearing in drilling data, used measured yield vs assumed values, and established a validated database, providing a robust foundation for ongoing mining.
The copper isotope ratios were measured in 42 mineral separates from the Cañariaco Norte porphyry copper deposit in northern Peru. Isotopic ratios ranged from -8.42‰ to 0.61‰, with near-surface iron oxides having the most depleted values and deeper chalcocite, covellite, and chalcopyrite having more typical hypogene ratios. The data indicate that most of the chalcocite and covellite formed from high-temperature hypogene processes, with only a minor portion resulting from supergene enrichment. The lack of an enriched isotopic signature suggests little potential for an extensive supergene enrichment blanket at depth due to the weathering history.
This document discusses developing a new metallogenic framework to aid mineral exploration in the Cobar Basin region of New South Wales, Australia. It involves creating metallogenic maps to better understand the timing, sources, and conditions of mineralization. This includes commodity studies, mineral potential studies, and developing mineral system models from the state to regional scale. Broken Hill and Cobar metallogenic syntheses projects are underway at 500k scales. The Cobar project involves new basement interpretations, metamorphic mapping with over 11,000 petrographic observations, and HyLogger studies on 9,000m of core to better understand alteration associated with mineralization.
The binding of cosmological structures by massless topological defectsSérgio Sacani
Assuming spherical symmetry and weak field, it is shown that if one solves the Poisson equation or the Einstein field
equations sourced by a topological defect, i.e. a singularity of a very specific form, the result is a localized gravitational
field capable of driving flat rotation (i.e. Keplerian circular orbits at a constant speed for all radii) of test masses on a thin
spherical shell without any underlying mass. Moreover, a large-scale structure which exploits this solution by assembling
concentrically a number of such topological defects can establish a flat stellar or galactic rotation curve, and can also deflect
light in the same manner as an equipotential (isothermal) sphere. Thus, the need for dark matter or modified gravity theory is
mitigated, at least in part.
EWOCS-I: The catalog of X-ray sources in Westerlund 1 from the Extended Weste...Sérgio Sacani
Context. With a mass exceeding several 104 M⊙ and a rich and dense population of massive stars, supermassive young star clusters
represent the most massive star-forming environment that is dominated by the feedback from massive stars and gravitational interactions
among stars.
Aims. In this paper we present the Extended Westerlund 1 and 2 Open Clusters Survey (EWOCS) project, which aims to investigate
the influence of the starburst environment on the formation of stars and planets, and on the evolution of both low and high mass stars.
The primary targets of this project are Westerlund 1 and 2, the closest supermassive star clusters to the Sun.
Methods. The project is based primarily on recent observations conducted with the Chandra and JWST observatories. Specifically,
the Chandra survey of Westerlund 1 consists of 36 new ACIS-I observations, nearly co-pointed, for a total exposure time of 1 Msec.
Additionally, we included 8 archival Chandra/ACIS-S observations. This paper presents the resulting catalog of X-ray sources within
and around Westerlund 1. Sources were detected by combining various existing methods, and photon extraction and source validation
were carried out using the ACIS-Extract software.
Results. The EWOCS X-ray catalog comprises 5963 validated sources out of the 9420 initially provided to ACIS-Extract, reaching a
photon flux threshold of approximately 2 × 10−8 photons cm−2
s
−1
. The X-ray sources exhibit a highly concentrated spatial distribution,
with 1075 sources located within the central 1 arcmin. We have successfully detected X-ray emissions from 126 out of the 166 known
massive stars of the cluster, and we have collected over 71 000 photons from the magnetar CXO J164710.20-455217.
More Related Content
Similar to Nickel and helium_evidence_for_melt_above_the_core_mantle_boundary
Role of trace elements in rare earth elementsPramoda Raj
Trace elements play an important role in igneous petrogenesis and can be used to understand magmatic processes. Trace elements are classified based on their behavior into incompatible and compatible elements. Rare earth elements (REE) are especially useful as their near-parallel patterns can indicate crystal fractionation. REE and other trace element analyses help determine the source depth of primary magmas and identify fractionating phases. Trace element discrimination diagrams also allow determination of paleotectonic settings. Overall, trace element studies provide insights into magma differentiation, source characterization, and petrogenetic modeling.
At the 2010 Prospector's and Developers Association of Canada (PDAC) Conference, David Lentz and Anthony Mariano gave a presentation on ranking and evaluating light to heavy rare earth deposits worldwide. This is that presentation.
Commerce Resources Corp. reports the results of a prospecting and sampling program completed on the Eldor Property. The results of this program are extremely encouraging, including the highest niobium mineralized sample collected to date from the area: 5.9% Nb2O5.
Role of Trace Elements In Petrogenesis Gokul Anand
Trace elements occur in very low concentrations in rocks and provide important information about magmatic processes. They can be classified as compatible or incompatible based on whether they fit easily into mantle mineral crystal structures. Geochemical analysis of trace elements using techniques like XRF and ICP-MS allows determination of magma source and depth, identification of fractionating phases, and testing of models of magmatic differentiation. Trace elements are especially useful for rare earth elements, which indicate the type of basalt and can identify fractionating phases from REE patterns.
The document provides an overview of mining potential and opportunities in the Philippines. It discusses the country's long history of mining dating back to the 16th century and rich diversity of metallic and non-metallic mineral resources. It highlights several major recent porphyry copper-gold discoveries, including the Far Southeast and Boyongan deposits. The minerals sector provides significant economic contributions and employment. Many areas remain underexplored and offer potential for further discoveries of copper, gold, and other mineral deposits.
The document summarizes the results of serpentinization of ultramafic rocks. There are three main products depending on the original rock composition: serpentinite and brucite from the serpentinization of dunites; serpentinite from the serpentinization of peridotites; and serpentinite and talc from the serpentinization of pyroxenites. Field studies in Guatemala identified dunite, lherzolite, and pyroxenite samples. Petrographic analysis found the rocks contain nickel-bearing minerals formed during serpentinization, including awaruite, pentlandite, and nickel-bearing serpentine and magnetite.
Nesosilicates or orthosilicates, have the orthosilicate ion, which constitute isolated (insular) [SiO4]4- tetrahedra that are connected only by interstitial cations. The atomic packing of the nesosilicate structure is generally dense which causes the mineral of this group to have relatively high specific gravity and hardness. The crystal habit of thee mineral is generally equidimensional and they have poor cleavage. The simplest structure in nesosilicates have mineral forsterite Mg2[SiO4]. These properties also that nesosilicates incorporate a considerable number of gemstones.
This document provides information about the mineral olivine. It begins with an introduction to olivine, noting its color and importance as a rock-forming mineral. It then discusses the members of the olivine family, their weathering, solid solution behavior, and position in Bowen's reaction series. The remainder of the document covers olivine's structure, alteration, high-pressure polymorphs, physical and optical properties, paragenesis, significance, and examples of occurrences. Diagrams and images supplement the detailed information presented.
This document provides background information on the Kalahari Craton in southern Africa, which consists of the Archaean Zimbabwe and Kaapvaal Cratons separated by the Limpopo Mobile Belt. It discusses the geological history and tectonic setting of the craton and its constituent terranes. The focus is on peridotite xenoliths from the Letlhakane kimberlite mine in northern Botswana, which will be studied to characterize the sub-cratonic lithospheric mantle beneath this region and better understand its origin and modification over time. A variety of analytical techniques will be used, including petrography, geochemistry, and Sm-Nd and Lu-Hf isotope analyses
This document provides an overview of talc mineralization in Nigeria. It discusses the geology of Nigeria and the formation of talc deposits. Talc deposits are found within Nigeria's schist belts in varied geologic and petrographic forms. Case studies of talc occurrences in locations like Wonu, Iseyin, Ilesha, and Isanlu are provided with details on the mineralization and rock associations at each site. The document concludes that talc deposits in Nigeria show marked variability in mineralization and petrographic properties.
[American mineralogist] a terrestrial magmatic hibonite grossite-vanadium ass...James AH Campbell
[American mineralogist] a terrestrial magmatic hibonite grossite-vanadium assemblage desilication and extreme reduction in a volcanic plumbing system mount carmel israel
A terrestrial magmatic hibonite grossite-vanadium assemblage desilication an...James AH Campbell
This document summarizes a study of a unique terrestrial occurrence of magmatic hibonite and grossite assemblages found in ejecta from Cretaceous pyroclastic deposits on Mount Carmel, Israel. The assemblages formed from calcium-aluminum rich silicate melts under extremely reducing conditions comparable to meteoritic counterparts. Textural evidence indicates hibonite first crystallized late after corundum and other phases, followed by grossite and spinel. Native vanadium spheres are included within hibonite, grossite and spinel, representing the most reduced conditions. Ongoing studies suggest the reducing conditions reflect interaction between basaltic magmas and mantle-derived methane-hydrogen fluids, resulting in
Highest niobium mineralized sample to date at MirannaStephan Bogner
Last week, the company reported sampling assays from the Miranna Area, located only 1 km east of its Ashram REE Deposit in Québec. The best results include 5.9% and 4.2% niobium pentoxide (Nb2O5). The 9 selected samples reported by Commerce averaged 2.3% Nb2O5. Of all 64 samples, 40 assayed >0.5% Nb2O5, with 16 surpassing 1%. Sampling also found significant grades of tantalum, phosphate and rare earth oxides (2 samples each graded >1,000 ppm Ta2O5 and 1% Nb2O5, while several samples revealed >10% P2O5).
When comparing these niobium grades with the range of global average mining grades of about 0.5 to 1.5% Nb2O5, and the average grades of niobium exploration projects, Commerce Resources indeed has every reason for being enthusiastic.
Niobium focused juniors seem to be enjoying a recent lift in share prices and market valuations potentially due to positive demand growth for niobium for structural steel for infrastructure projects, as well as for the current lighter and stronger chassis for cars. MDN Inc. has recently seen its’ share price appreciate by almost 400% following the announcement of their acquisition of the James Bay Niobium Project, called the Argor Project, which has an historic indicated resource with a grade of 0.52% Nb2O5.
Last year, NioCorp Developments Ltd. (originally structured by Zimtu Capital Corp.) reported an average indicated resource grade of 0.71% Nb2O5 assuming a 0.3% cut-off grade at its Elk Creek Niobium Deposit in Nebraska, USA. Today, NioCorp enjoys a market valuation exceeding $150 million CAD.
The document summarizes a study of the Groote Eylandt manganese orebody in Australia. The objectives of the study were to construct an accurate resource/reserve model using over 5,500 drill holes to satisfy reporting standards. Previous models were outdated and inaccurate. Key challenges included the orebody's variability and complex geological history. The new model incorporated stratigraphic units, addressed issues like downhole smearing in drilling data, used measured yield vs assumed values, and established a validated database, providing a robust foundation for ongoing mining.
The copper isotope ratios were measured in 42 mineral separates from the Cañariaco Norte porphyry copper deposit in northern Peru. Isotopic ratios ranged from -8.42‰ to 0.61‰, with near-surface iron oxides having the most depleted values and deeper chalcocite, covellite, and chalcopyrite having more typical hypogene ratios. The data indicate that most of the chalcocite and covellite formed from high-temperature hypogene processes, with only a minor portion resulting from supergene enrichment. The lack of an enriched isotopic signature suggests little potential for an extensive supergene enrichment blanket at depth due to the weathering history.
This document discusses developing a new metallogenic framework to aid mineral exploration in the Cobar Basin region of New South Wales, Australia. It involves creating metallogenic maps to better understand the timing, sources, and conditions of mineralization. This includes commodity studies, mineral potential studies, and developing mineral system models from the state to regional scale. Broken Hill and Cobar metallogenic syntheses projects are underway at 500k scales. The Cobar project involves new basement interpretations, metamorphic mapping with over 11,000 petrographic observations, and HyLogger studies on 9,000m of core to better understand alteration associated with mineralization.
Similar to Nickel and helium_evidence_for_melt_above_the_core_mantle_boundary (20)
The binding of cosmological structures by massless topological defectsSérgio Sacani
Assuming spherical symmetry and weak field, it is shown that if one solves the Poisson equation or the Einstein field
equations sourced by a topological defect, i.e. a singularity of a very specific form, the result is a localized gravitational
field capable of driving flat rotation (i.e. Keplerian circular orbits at a constant speed for all radii) of test masses on a thin
spherical shell without any underlying mass. Moreover, a large-scale structure which exploits this solution by assembling
concentrically a number of such topological defects can establish a flat stellar or galactic rotation curve, and can also deflect
light in the same manner as an equipotential (isothermal) sphere. Thus, the need for dark matter or modified gravity theory is
mitigated, at least in part.
EWOCS-I: The catalog of X-ray sources in Westerlund 1 from the Extended Weste...Sérgio Sacani
Context. With a mass exceeding several 104 M⊙ and a rich and dense population of massive stars, supermassive young star clusters
represent the most massive star-forming environment that is dominated by the feedback from massive stars and gravitational interactions
among stars.
Aims. In this paper we present the Extended Westerlund 1 and 2 Open Clusters Survey (EWOCS) project, which aims to investigate
the influence of the starburst environment on the formation of stars and planets, and on the evolution of both low and high mass stars.
The primary targets of this project are Westerlund 1 and 2, the closest supermassive star clusters to the Sun.
Methods. The project is based primarily on recent observations conducted with the Chandra and JWST observatories. Specifically,
the Chandra survey of Westerlund 1 consists of 36 new ACIS-I observations, nearly co-pointed, for a total exposure time of 1 Msec.
Additionally, we included 8 archival Chandra/ACIS-S observations. This paper presents the resulting catalog of X-ray sources within
and around Westerlund 1. Sources were detected by combining various existing methods, and photon extraction and source validation
were carried out using the ACIS-Extract software.
Results. The EWOCS X-ray catalog comprises 5963 validated sources out of the 9420 initially provided to ACIS-Extract, reaching a
photon flux threshold of approximately 2 × 10−8 photons cm−2
s
−1
. The X-ray sources exhibit a highly concentrated spatial distribution,
with 1075 sources located within the central 1 arcmin. We have successfully detected X-ray emissions from 126 out of the 166 known
massive stars of the cluster, and we have collected over 71 000 photons from the magnetar CXO J164710.20-455217.
The debris of the ‘last major merger’ is dynamically youngSérgio Sacani
The Milky Way’s (MW) inner stellar halo contains an [Fe/H]-rich component with highly eccentric orbits, often referred to as the
‘last major merger.’ Hypotheses for the origin of this component include Gaia-Sausage/Enceladus (GSE), where the progenitor
collided with the MW proto-disc 8–11 Gyr ago, and the Virgo Radial Merger (VRM), where the progenitor collided with the
MW disc within the last 3 Gyr. These two scenarios make different predictions about observable structure in local phase space,
because the morphology of debris depends on how long it has had to phase mix. The recently identified phase-space folds in Gaia
DR3 have positive caustic velocities, making them fundamentally different than the phase-mixed chevrons found in simulations
at late times. Roughly 20 per cent of the stars in the prograde local stellar halo are associated with the observed caustics. Based
on a simple phase-mixing model, the observed number of caustics are consistent with a merger that occurred 1–2 Gyr ago.
We also compare the observed phase-space distribution to FIRE-2 Latte simulations of GSE-like mergers, using a quantitative
measurement of phase mixing (2D causticality). The observed local phase-space distribution best matches the simulated data
1–2 Gyr after collision, and certainly not later than 3 Gyr. This is further evidence that the progenitor of the ‘last major merger’
did not collide with the MW proto-disc at early times, as is thought for the GSE, but instead collided with the MW disc within
the last few Gyr, consistent with the body of work surrounding the VRM.
Observation of Io’s Resurfacing via Plume Deposition Using Ground-based Adapt...Sérgio Sacani
Since volcanic activity was first discovered on Io from Voyager images in 1979, changes
on Io’s surface have been monitored from both spacecraft and ground-based telescopes.
Here, we present the highest spatial resolution images of Io ever obtained from a groundbased telescope. These images, acquired by the SHARK-VIS instrument on the Large
Binocular Telescope, show evidence of a major resurfacing event on Io’s trailing hemisphere. When compared to the most recent spacecraft images, the SHARK-VIS images
show that a plume deposit from a powerful eruption at Pillan Patera has covered part
of the long-lived Pele plume deposit. Although this type of resurfacing event may be common on Io, few have been detected due to the rarity of spacecraft visits and the previously low spatial resolution available from Earth-based telescopes. The SHARK-VIS instrument ushers in a new era of high resolution imaging of Io’s surface using adaptive
optics at visible wavelengths.
Earliest Galaxies in the JADES Origins Field: Luminosity Function and Cosmic ...Sérgio Sacani
We characterize the earliest galaxy population in the JADES Origins Field (JOF), the deepest
imaging field observed with JWST. We make use of the ancillary Hubble optical images (5 filters
spanning 0.4−0.9µm) and novel JWST images with 14 filters spanning 0.8−5µm, including 7 mediumband filters, and reaching total exposure times of up to 46 hours per filter. We combine all our data
at > 2.3µm to construct an ultradeep image, reaching as deep as ≈ 31.4 AB mag in the stack and
30.3-31.0 AB mag (5σ, r = 0.1” circular aperture) in individual filters. We measure photometric
redshifts and use robust selection criteria to identify a sample of eight galaxy candidates at redshifts
z = 11.5 − 15. These objects show compact half-light radii of R1/2 ∼ 50 − 200pc, stellar masses of
M⋆ ∼ 107−108M⊙, and star-formation rates of SFR ∼ 0.1−1 M⊙ yr−1
. Our search finds no candidates
at 15 < z < 20, placing upper limits at these redshifts. We develop a forward modeling approach to
infer the properties of the evolving luminosity function without binning in redshift or luminosity that
marginalizes over the photometric redshift uncertainty of our candidate galaxies and incorporates the
impact of non-detections. We find a z = 12 luminosity function in good agreement with prior results,
and that the luminosity function normalization and UV luminosity density decline by a factor of ∼ 2.5
from z = 12 to z = 14. We discuss the possible implications of our results in the context of theoretical
models for evolution of the dark matter halo mass function.
THE IMPORTANCE OF MARTIAN ATMOSPHERE SAMPLE RETURN.Sérgio Sacani
The return of a sample of near-surface atmosphere from Mars would facilitate answers to several first-order science questions surrounding the formation and evolution of the planet. One of the important aspects of terrestrial planet formation in general is the role that primary atmospheres played in influencing the chemistry and structure of the planets and their antecedents. Studies of the martian atmosphere can be used to investigate the role of a primary atmosphere in its history. Atmosphere samples would also inform our understanding of the near-surface chemistry of the planet, and ultimately the prospects for life. High-precision isotopic analyses of constituent gases are needed to address these questions, requiring that the analyses are made on returned samples rather than in situ.
Multi-source connectivity as the driver of solar wind variability in the heli...Sérgio Sacani
The ambient solar wind that flls the heliosphere originates from multiple
sources in the solar corona and is highly structured. It is often described
as high-speed, relatively homogeneous, plasma streams from coronal
holes and slow-speed, highly variable, streams whose source regions are
under debate. A key goal of ESA/NASA’s Solar Orbiter mission is to identify
solar wind sources and understand what drives the complexity seen in the
heliosphere. By combining magnetic feld modelling and spectroscopic
techniques with high-resolution observations and measurements, we show
that the solar wind variability detected in situ by Solar Orbiter in March
2022 is driven by spatio-temporal changes in the magnetic connectivity to
multiple sources in the solar atmosphere. The magnetic feld footpoints
connected to the spacecraft moved from the boundaries of a coronal hole
to one active region (12961) and then across to another region (12957). This
is refected in the in situ measurements, which show the transition from fast
to highly Alfvénic then to slow solar wind that is disrupted by the arrival of
a coronal mass ejection. Our results describe solar wind variability at 0.5 au
but are applicable to near-Earth observatories.
Gliese 12 b: A Temperate Earth-sized Planet at 12 pc Ideal for Atmospheric Tr...Sérgio Sacani
Recent discoveries of Earth-sized planets transiting nearby M dwarfs have made it possible to characterize the
atmospheres of terrestrial planets via follow-up spectroscopic observations. However, the number of such planets
receiving low insolation is still small, limiting our ability to understand the diversity of the atmospheric
composition and climates of temperate terrestrial planets. We report the discovery of an Earth-sized planet
transiting the nearby (12 pc) inactive M3.0 dwarf Gliese 12 (TOI-6251) with an orbital period (Porb) of 12.76 days.
The planet, Gliese 12 b, was initially identified as a candidate with an ambiguous Porb from TESS data. We
confirmed the transit signal and Porb using ground-based photometry with MuSCAT2 and MuSCAT3, and
validated the planetary nature of the signal using high-resolution images from Gemini/NIRI and Keck/NIRC2 as
well as radial velocity (RV) measurements from the InfraRed Doppler instrument on the Subaru 8.2 m telescope
and from CARMENES on the CAHA 3.5 m telescope. X-ray observations with XMM-Newton showed the host
star is inactive, with an X-ray-to-bolometric luminosity ratio of log 5.7 L L X bol » - . Joint analysis of the light
curves and RV measurements revealed that Gliese 12 b has a radius of 0.96 ± 0.05 R⊕,a3σ mass upper limit of
3.9 M⊕, and an equilibrium temperature of 315 ± 6 K assuming zero albedo. The transmission spectroscopy metric
(TSM) value of Gliese 12 b is close to the TSM values of the TRAPPIST-1 planets, adding Gliese 12 b to the small
list of potentially terrestrial, temperate planets amenable to atmospheric characterization with JWST.
Gliese 12 b, a temperate Earth-sized planet at 12 parsecs discovered with TES...Sérgio Sacani
We report on the discovery of Gliese 12 b, the nearest transiting temperate, Earth-sized planet found to date. Gliese 12 is a
bright (V = 12.6 mag, K = 7.8 mag) metal-poor M4V star only 12.162 ± 0.005 pc away from the Solar system with one of the
lowest stellar activity levels known for M-dwarfs. A planet candidate was detected by TESS based on only 3 transits in sectors
42, 43, and 57, with an ambiguity in the orbital period due to observational gaps. We performed follow-up transit observations
with CHEOPS and ground-based photometry with MINERVA-Australis, SPECULOOS, and Purple Mountain Observatory,
as well as further TESS observations in sector 70. We statistically validate Gliese 12 b as a planet with an orbital period of
12.76144 ± 0.00006 d and a radius of 1.0 ± 0.1 R⊕, resulting in an equilibrium temperature of ∼315 K. Gliese 12 b has excellent
future prospects for precise mass measurement, which may inform how planetary internal structure is affected by the stellar
compositional environment. Gliese 12 b also represents one of the best targets to study whether Earth-like planets orbiting cool
stars can retain their atmospheres, a crucial step to advance our understanding of habitability on Earth and across the galaxy.
The importance of continents, oceans and plate tectonics for the evolution of...Sérgio Sacani
Within the uncertainties of involved astronomical and biological parameters, the Drake Equation
typically predicts that there should be many exoplanets in our galaxy hosting active, communicative
civilizations (ACCs). These optimistic calculations are however not supported by evidence, which is
often referred to as the Fermi Paradox. Here, we elaborate on this long-standing enigma by showing
the importance of planetary tectonic style for biological evolution. We summarize growing evidence
that a prolonged transition from Mesoproterozoic active single lid tectonics (1.6 to 1.0 Ga) to modern
plate tectonics occurred in the Neoproterozoic Era (1.0 to 0.541 Ga), which dramatically accelerated
emergence and evolution of complex species. We further suggest that both continents and oceans
are required for ACCs because early evolution of simple life must happen in water but late evolution
of advanced life capable of creating technology must happen on land. We resolve the Fermi Paradox
(1) by adding two additional terms to the Drake Equation: foc
(the fraction of habitable exoplanets
with significant continents and oceans) and fpt
(the fraction of habitable exoplanets with significant
continents and oceans that have had plate tectonics operating for at least 0.5 Ga); and (2) by
demonstrating that the product of foc
and fpt
is very small (< 0.00003–0.002). We propose that the lack
of evidence for ACCs reflects the scarcity of long-lived plate tectonics and/or continents and oceans on
exoplanets with primitive life.
A Giant Impact Origin for the First Subduction on EarthSérgio Sacani
Hadean zircons provide a potential record of Earth's earliest subduction 4.3 billion years ago. Itremains enigmatic how subduction could be initiated so soon after the presumably Moon‐forming giant impact(MGI). Earlier studies found an increase in Earth's core‐mantle boundary (CMB) temperature due to theaccumulation of the impactor's core, and our recent work shows Earth's lower mantle remains largely solid, withsome of the impactor's mantle potentially surviving as the large low‐shear velocity provinces (LLSVPs). Here,we show that a hot post‐impact CMB drives the initiation of strong mantle plumes that can induce subductioninitiation ∼200 Myr after the MGI. 2D and 3D thermomechanical computations show that a high CMBtemperature is the primary factor triggering early subduction, with enrichment of heat‐producing elements inLLSVPs as another potential factor. The models link the earliest subduction to the MGI with implications forunderstanding the diverse tectonic regimes of rocky planets.
Climate extremes likely to drive land mammal extinction during next supercont...Sérgio Sacani
Mammals have dominated Earth for approximately 55 Myr thanks to their
adaptations and resilience to warming and cooling during the Cenozoic. All
life will eventually perish in a runaway greenhouse once absorbed solar
radiation exceeds the emission of thermal radiation in several billions of
years. However, conditions rendering the Earth naturally inhospitable to
mammals may develop sooner because of long-term processes linked to
plate tectonics (short-term perturbations are not considered here). In
~250 Myr, all continents will converge to form Earth’s next supercontinent,
Pangea Ultima. A natural consequence of the creation and decay of Pangea
Ultima will be extremes in pCO2 due to changes in volcanic rifting and
outgassing. Here we show that increased pCO2, solar energy (F⨀;
approximately +2.5% W m−2 greater than today) and continentality (larger
range in temperatures away from the ocean) lead to increasing warming
hostile to mammalian life. We assess their impact on mammalian
physiological limits (dry bulb, wet bulb and Humidex heat stress indicators)
as well as a planetary habitability index. Given mammals’ continued survival,
predicted background pCO2 levels of 410–816 ppm combined with increased
F⨀ will probably lead to a climate tipping point and their mass extinction.
The results also highlight how global landmass configuration, pCO2 and F⨀
play a critical role in planetary habitability.
Constraints on Neutrino Natal Kicks from Black-Hole Binary VFTS 243Sérgio Sacani
The recently reported observation of VFTS 243 is the first example of a massive black-hole binary
system with negligible binary interaction following black-hole formation. The black-hole mass (≈10M⊙)
and near-circular orbit (e ≈ 0.02) of VFTS 243 suggest that the progenitor star experienced complete
collapse, with energy-momentum being lost predominantly through neutrinos. VFTS 243 enables us to
constrain the natal kick and neutrino-emission asymmetry during black-hole formation. At 68% confidence
level, the natal kick velocity (mass decrement) is ≲10 km=s (≲1.0M⊙), with a full probability distribution
that peaks when ≈0.3M⊙ were ejected, presumably in neutrinos, and the black hole experienced a natal
kick of 4 km=s. The neutrino-emission asymmetry is ≲4%, with best fit values of ∼0–0.2%. Such a small
neutrino natal kick accompanying black-hole formation is in agreement with theoretical predictions.
Detectability of Solar Panels as a TechnosignatureSérgio Sacani
In this work, we assess the potential detectability of solar panels made of silicon on an Earth-like
exoplanet as a potential technosignature. Silicon-based photovoltaic cells have high reflectance in the
UV-VIS and in the near-IR, within the wavelength range of a space-based flagship mission concept
like the Habitable Worlds Observatory (HWO). Assuming that only solar energy is used to provide
the 2022 human energy needs with a land cover of ∼ 2.4%, and projecting the future energy demand
assuming various growth-rate scenarios, we assess the detectability with an 8 m HWO-like telescope.
Assuming the most favorable viewing orientation, and focusing on the strong absorption edge in the
ultraviolet-to-visible (0.34 − 0.52 µm), we find that several 100s of hours of observation time is needed
to reach a SNR of 5 for an Earth-like planet around a Sun-like star at 10pc, even with a solar panel
coverage of ∼ 23% land coverage of a future Earth. We discuss the necessity of concepts like Kardeshev
Type I/II civilizations and Dyson spheres, which would aim to harness vast amounts of energy. Even
with much larger populations than today, the total energy use of human civilization would be orders of
magnitude below the threshold for causing direct thermal heating or reaching the scale of a Kardashev
Type I civilization. Any extraterrrestrial civilization that likewise achieves sustainable population
levels may also find a limit on its need to expand, which suggests that a galaxy-spanning civilization
as imagined in the Fermi paradox may not exist.
Jet reorientation in central galaxies of clusters and groups: insights from V...Sérgio Sacani
Recent observations of galaxy clusters and groups with misalignments between their central AGN jets
and X-ray cavities, or with multiple misaligned cavities, have raised concerns about the jet – bubble
connection in cooling cores, and the processes responsible for jet realignment. To investigate the
frequency and causes of such misalignments, we construct a sample of 16 cool core galaxy clusters and
groups. Using VLBA radio data we measure the parsec-scale position angle of the jets, and compare
it with the position angle of the X-ray cavities detected in Chandra data. Using the overall sample
and selected subsets, we consistently find that there is a 30% – 38% chance to find a misalignment
larger than ∆Ψ = 45◦ when observing a cluster/group with a detected jet and at least one cavity. We
determine that projection may account for an apparently large ∆Ψ only in a fraction of objects (∼35%),
and given that gas dynamical disturbances (as sloshing) are found in both aligned and misaligned
systems, we exclude environmental perturbation as the main driver of cavity – jet misalignment.
Moreover, we find that large misalignments (up to ∼ 90◦
) are favored over smaller ones (45◦ ≤ ∆Ψ ≤
70◦
), and that the change in jet direction can occur on timescales between one and a few tens of Myr.
We conclude that misalignments are more likely related to actual reorientation of the jet axis, and we
discuss several engine-based mechanisms that may cause these dramatic changes.
The solar dynamo begins near the surfaceSérgio Sacani
The magnetic dynamo cycle of the Sun features a distinct pattern: a propagating
region of sunspot emergence appears around 30° latitude and vanishes near the
equator every 11 years (ref. 1). Moreover, longitudinal flows called torsional oscillations
closely shadow sunspot migration, undoubtedly sharing a common cause2. Contrary
to theories suggesting deep origins of these phenomena, helioseismology pinpoints
low-latitude torsional oscillations to the outer 5–10% of the Sun, the near-surface
shear layer3,4. Within this zone, inwardly increasing differential rotation coupled with
a poloidal magnetic field strongly implicates the magneto-rotational instability5,6,
prominent in accretion-disk theory and observed in laboratory experiments7.
Together, these two facts prompt the general question: whether the solar dynamo is
possibly a near-surface instability. Here we report strong affirmative evidence in stark
contrast to traditional models8 focusing on the deeper tachocline. Simple analytic
estimates show that the near-surface magneto-rotational instability better explains
the spatiotemporal scales of the torsional oscillations and inferred subsurface
magnetic field amplitudes9. State-of-the-art numerical simulations corroborate these
estimates and reproduce hemispherical magnetic current helicity laws10. The dynamo
resulting from a well-understood near-surface phenomenon improves prospects
for accurate predictions of full magnetic cycles and space weather, affecting the
electromagnetic infrastructure of Earth.
Extensive Pollution of Uranus and Neptune’s Atmospheres by Upsweep of Icy Mat...Sérgio Sacani
In the Nice model of solar system formation, Uranus and Neptune undergo an orbital upheaval,
sweeping through a planetesimal disk. The region of the disk from which material is accreted by
the ice giants during this phase of their evolution has not previously been identified. We perform
direct N-body orbital simulations of the four giant planets to determine the amount and origin of solid
accretion during this orbital upheaval. We find that the ice giants undergo an extreme bombardment
event, with collision rates as much as ∼3 per hour assuming km-sized planetesimals, increasing the
total planet mass by up to ∼0.35%. In all cases, the initially outermost ice giant experiences the
largest total enhancement. We determine that for some plausible planetesimal properties, the resulting
atmospheric enrichment could potentially produce sufficient latent heat to alter the planetary cooling
timescale according to existing models. Our findings suggest that substantial accretion during this
phase of planetary evolution may have been sufficient to impact the atmospheric composition and
thermal evolution of the ice giants, motivating future work on the fate of deposited solid material.
Exomoons & Exorings with the Habitable Worlds Observatory I: On the Detection...Sérgio Sacani
The highest priority recommendation of the Astro2020 Decadal Survey for space-based astronomy
was the construction of an observatory capable of characterizing habitable worlds. In this paper series
we explore the detectability of and interference from exomoons and exorings serendipitously observed
with the proposed Habitable Worlds Observatory (HWO) as it seeks to characterize exoplanets, starting
in this manuscript with Earth-Moon analog mutual events. Unlike transits, which only occur in systems
viewed near edge-on, shadow (i.e., solar eclipse) and lunar eclipse mutual events occur in almost every
star-planet-moon system. The cadence of these events can vary widely from ∼yearly to multiple events
per day, as was the case in our younger Earth-Moon system. Leveraging previous space-based (EPOXI)
lightcurves of a Moon transit and performance predictions from the LUVOIR-B concept, we derive
the detectability of Moon analogs with HWO. We determine that Earth-Moon analogs are detectable
with observation of ∼2-20 mutual events for systems within 10 pc, and larger moons should remain
detectable out to 20 pc. We explore the extent to which exomoon mutual events can mimic planet
features and weather. We find that HWO wavelength coverage in the near-IR, specifically in the 1.4 µm
water band where large moons can outshine their host planet, will aid in differentiating exomoon signals
from exoplanet variability. Finally, we predict that exomoons formed through collision processes akin
to our Moon are more likely to be detected in younger systems, where shorter orbital periods and
favorable geometry enhance the probability and frequency of mutual events.
Emergent ribozyme behaviors in oxychlorine brines indicate a unique niche for...Sérgio Sacani
Mars is a particularly attractive candidate among known astronomical objects
to potentially host life. Results from space exploration missions have provided
insights into Martian geochemistry that indicate oxychlorine species, particularly perchlorate, are ubiquitous features of the Martian geochemical landscape. Perchlorate presents potential obstacles for known forms of life due to
its toxicity. However, it can also provide potential benefits, such as producing
brines by deliquescence, like those thought to exist on present-day Mars. Here
we show perchlorate brines support folding and catalysis of functional RNAs,
while inactivating representative protein enzymes. Additionally, we show
perchlorate and other oxychlorine species enable ribozyme functions,
including homeostasis-like regulatory behavior and ribozyme-catalyzed
chlorination of organic molecules. We suggest nucleic acids are uniquely wellsuited to hypersaline Martian environments. Furthermore, Martian near- or
subsurface oxychlorine brines, and brines found in potential lifeforms, could
provide a unique niche for biomolecular evolution.
Continuum emission from within the plunging region of black hole discsSérgio Sacani
The thermal continuum emission observed from accreting black holes across X-ray bands has the potential to be leveraged as a
powerful probe of the mass and spin of the central black hole. The vast majority of existing ‘continuum fitting’ models neglect
emission sourced at and within the innermost stable circular orbit (ISCO) of the black hole. Numerical simulations, however,
find non-zero emission sourced from these regions. In this work, we extend existing techniques by including the emission
sourced from within the plunging region, utilizing new analytical models that reproduce the properties of numerical accretion
simulations. We show that in general the neglected intra-ISCO emission produces a hot-and-small quasi-blackbody component,
but can also produce a weak power-law tail for more extreme parameter regions. A similar hot-and-small blackbody component
has been added in by hand in an ad hoc manner to previous analyses of X-ray binary spectra. We show that the X-ray spectrum
of MAXI J1820+070 in a soft-state outburst is extremely well described by a full Kerr black hole disc, while conventional
models that neglect intra-ISCO emission are unable to reproduce the data. We believe this represents the first robust detection of
intra-ISCO emission in the literature, and allows additional constraints to be placed on the MAXI J1820 + 070 black hole spin
which must be low a• < 0.5 to allow a detectable intra-ISCO region. Emission from within the ISCO is the dominant emission
component in the MAXI J1820 + 070 spectrum between 6 and 10 keV, highlighting the necessity of including this region. Our
continuum fitting model is made publicly available.