Mass Loss Rate Research Articles

Hot subdwarf wind models with accurate abundances

Context. Helium-dominated subdwarfs are core helium burning stars stripped of their envelope. The nuclear evolution of these stars alters surface abundances. Modified abundances impact the strength of the stellar wind. Aims. We aim to understand the influence of modified surface abundances on the strength of the stellar wind in the helium-dominated subdwarfs CD–46 8926 and CD–51 11879. A modified wind strength could resolve the problem with the X-ray emission of these stars, as the expected X-ray luminosity of both stars is significantly higher than the upper limit determined from observations. Methods. We used our own optical spectroscopy combined with archival ultraviolet spectroscopy and photometry to derive basic parameters and surface abundances of selected subdwarfs. The resulting parameterst served as input for the METUJE stellar wind code, which predicts the wind structure of these stars. We compared the derived wind parameters with the predictions derived for solar abundances. Results. The optical analysis showed that both subdwarfs have effective temperatures in excess of 60 kK and a strong overabundance of carbon in the case of CD–46 8926 and nitrogen in the case of CD–51 11879. We interpret the abundance patterns as being a result of enrichment by the products of nuclear reactions. The modified abundances reduce the wind mass-loss rate by tens of percent. The reduction improves the predicted wind line profiles in comparison to observations. The change in helium abundance does not have a strong effect on the wind parameters. As a result of a lower estimated bolometric luminosity and mass-loss rate and a larger distance, the expected X-ray luminosities become lower and agree with observational upper limits. Conclusions. The nucleosynthesis does not significantly alter the strength of the wind of hot subdwarfs, but the inclusion of proper stellar parameters improves the agreement with observational wind characteristics. Our analysis indicates that subdwarfs overabundant in helium are typically able to launch wind. This conclusion is supported by data gathered for thousands of subdwarfs from the literature, which shows that subdwarfs overabundant in helium avoid the region in the Kiel diagram where the winds are predicted to be absent. This can be interpreted in terms of the gravitational settling of helium, which is suppressed by the winds.

The elusive atmosphere of WASP–12 b

To date, the hot Jupiter WASP–12 b has been the only planet with confirmed orbital decay. The late F-type host star has been hypothesized to be surrounded by a large structure of circumstellar material evaporated from the planet. We obtained two high-resolution spectral transit time series with CARMENES and extensively searched for absorption signals by the atomic species Na, H, Ca, and He using transmission spectroscopy, thereby covering the He I λ10833 Å triplet with high resolution for the first time. We apply SYSREM for atomic line transmission spectroscopy, introduce the technique of signal protection to improve the results for individual absorption lines, and compare the outcomes to those of established methods. No transmission signals were detected and the most stringent upper limits as of yet were derived for the individual indicators. Nonetheless, we found variation in the stellar Hα and He I λ10833 Å lines, the origin of which remains uncertain but is unlikely to be activity. To constrain the enigmatic activity state of WASP–12, we analyzed XMM-Newton X-ray data and found the star to be moderately active at most. We deduced an upper limit for the X-ray luminosity and the irradiating X-ray and extreme ultraviolet (XUV) flux of WASP–12 b. Based on the XUV flux upper limit and the lack of the He I λ10833 Å signal, our hydrodynamic models slightly favor a moderately irradiated planet with a thermospheric temperature of ≲12 000 K, and a conservative upper limit of ≲4 × 1012 g s−1 on the mass-loss rate. Our study does not provide evidence for an extended planetary atmosphere or absorption by circumstellar material close to the planetary orbit.

Binary Interaction Can Yield a Diversity of Circumstellar Media around Type II Supernova Progenitors

Recent observations of supernovae (SNe) have indicated that a fraction of massive stars possess dense circumstellar medium (CSM) at the moment of their core collapses. They suggest the presence of additional activities of the SN progenitor driving the enhancement of the mass-loss rate, and some physical processes attributing to a single star’s activities have been considered. In this study, we carry out binary evolutionary simulations of massive stars by MESA and investigate effects on the subsequent CSM formation through hydrodynamical simulations by PLUTO. We show that the mass transfer rate in a binary can increase at the beginning of the Roche lobe overflow, and this enhancement would be associated with the structure of the CSM before the explosion. We also illustrate that, depending on the orbital period of the binary, the density structure of the CSM can have a diverse distribution, including shell-like and cliff-like structures. These characteristic structures appear within the length scale of ∼1017 cm and could be traced by long-term observations of SNe, if the slow velocity of the CSM is assumed (∼10 km s−1). Our results highlight the importance of binary interaction in the aspect of reproducing the diversity of the CSM configuration.

A far-ultraviolet-driven photoevaporation flow observed in a protoplanetary disk.

Most low-mass stars form in stellar clusters that also contain massive stars, which are sources of far-ultraviolet (FUV) radiation. Theoretical models predict that this FUV radiation produces photodissociation regions (PDRs) on the surfaces of protoplanetary disks around low-mass stars, which affects planet formation within the disks. We report James Webb Space Telescope and Atacama Large Millimeter Array observations of a FUV-irradiated protoplanetary disk in the Orion Nebula. Emission lines are detected from the PDR; modeling their kinematics and excitation allowed us to constrain the physical conditions within the gas. We quantified the mass-loss rate induced by the FUV irradiation and found that it is sufficient to remove gas from the disk in less than a million years. This is rapid enough to affect giant planet formation in the disk.

Circumstellar interaction models for the early bolometric light curve of SN 2023ixf

Type II supernovae (SNe II) show growing evidence of an interaction with circumstellar material (CSM) surrounding their progenitor stars as a consequence of enhanced mass loss during the last years of the progenitor’s life, although the exact mechanism is still unknown. We present an analysis of the progenitor mass-loss history of SN 2023ixf, a nearby SN II showing signs of an interaction. First, we calculated the early-time (< 19 days) bolometric light curve for SN 2023ixf based on the integration of the observed flux covering ultraviolet, optical and near-infrared bands, and black-body extrapolations for the unobserved flux. Our calculations detected the sudden increase to maximum luminosity and temperature, in addition to the subsequent fall, displaying an evident peak. This is the first time that this phase can be precisely estimated for a SN II. We used the early-time bolometric light curve of SN 2023ixf to test the calibrations of bolometric corrections against colours from the literature. In addition, we included the observations of SN 2023ixf into some of the available calibrations to extend their use to earlier epochs. A comparison of the observed bolometric light curve to SN II explosion models with CSM interaction suggests a progenitor mass-loss rate of Ṁ = 3 × 10−3 M⊙ yr−1 confined to 12 000 R⊙ (∼8 × 1014 cm) and a wind acceleration parameter of β = 5. This model reproduces the early bolometric light curve, expansion velocities, and the epoch of disappearance of interacting lines in the spectra. This model indicates that the wind was launched ∼80 yr before the explosion. If the effect of the wind acceleration is not taken into account, the enhanced wind must have developed over the final months to years prior to the SN, which may not be consistent with the lack of outburst detection in pre-explosion images over the last ∼20 yr before explosion.

A Large and Variable Leading Tail of Helium in a Hot Saturn Undergoing Runaway Inflation

Atmospheric escape shapes the fate of exoplanets, with statistical evidence for transformative mass loss imprinted across the mass–radius–insolation distribution. Here, we present transit spectroscopy of the highly irradiated, low-gravity, inflated hot Saturn HAT-P-67 b. The Habitable Zone Planet Finder spectra show a detection of up to 10% absorption depth of the 10833 Å helium triplet. The 13.8 hr of on-sky integration time over 39 nights sample the entire planet orbit, uncovering excess helium absorption preceding the transit by up to 130 planetary radii in a large leading tail. This configuration can be understood as the escaping material overflowing its small Roche lobe and advecting most of the gas into the stellar—and not planetary—rest frame, consistent with the Doppler velocity structure seen in the helium line profiles. The prominent leading tail serves as direct evidence for dayside mass loss with a strong day-/nightside asymmetry. We see some transit-to-transit variability in the line profile, consistent with the interplay of stellar and planetary winds. We employ one-dimensional Parker wind models to estimate the mass-loss rate, finding values on the order of 2 × 1013 g s−1, with large uncertainties owing to the unknown X-ray and ultraviolet (XUV) flux of the F host star. The large mass loss in HAT-P-67 b represents a valuable example of an inflated hot Saturn, a class of planets recently identified to be rare, as their atmospheres are predicted to evaporate quickly. We contrast two physical mechanisms for runaway evaporation: ohmic dissipation and XUV irradiation, slightly favoring the latter.

The effect of winds on atmospheric layers of red supergiants II. Modelling VLTI/GRAVITY and MATISSE observations of AH Sco, KW Sgr, V602 Car, CK Car, and V460 Car

Context. Mass loss plays a crucial role in the lives of massive stars, especially as the star leaves the main sequence and evolves to the red supergiant (RSG) phase. Despite its importance, the physical processes that trigger mass-loss events in RSGs are still not well understood. Recently, we showed that adding a semi-empirical wind to atmosphere models can accurately reproduce observed extensions in the atmospheres of RSGs, where the mass-loss events are taking place, particularly in the CO and water lines. Aims. By adding a static wind to a MARCS atmospheric model, we computed synthetic observables that match new interferometric data of the RSGs AH Sco, KW Sgr, V602 Car, CK Car, and V460 Car obtained with the VLTI/MATISSE and VLTI/GRAVITY instruments between August 2022 and February 2023. We also used archival VLTI/AMBER data of KW Sgr and VLTI/GRAVITY data of AH Sco. The MATISSE wavelength range includes the SiO molecule at 4.0 μm with a spectral resolution of R ~ 500. Methods. The model intensities with respect to the line-of-sight angle (μ) as well as the spectra and visibilities were computed using the stellar radiative transfer code TURBOSPECTRUM. We found the best-fit model, mass-loss rate, and best-fit angular Rosseland diameter for the observations. We simultaneously matched our model to the data, covering a wavelength range of 1.8–5.0 μm, which corresponds to the K, L, and M bands. Results. Our models reproduce the spectro-interferometric data over this wide wavelength range, including extended atmospheric layers of CO, H2O, and SiO. We obtain a range of Rosseland angular diameters between 3.0 < θRoss < 5.5 mas and a range of mass-loss rates of −6.5 < log Ṁ/M⊙ yr−1 < −4 for our five targets. In our best-fit models, the partial pressure of SiO relative to the gas pressure, PSiO/Pg, and the SiO 4.0 μm line intensity increase between 2 and 3 stellar radii. The relative intensity depends on the luminosity used for our models, since the more luminous models have a higher mass-loss rate. Conclusions. This work further demonstrates that our MARCS+wind model can reproduce the observed physical extension of RSG atmospheres for several spectral diagnostics spanning a broad wavelength range. We reproduce both spectra and visibilities of newly obtained data as well as provide temperature and density stratifications that are consistent with the observations. With the MATISSE data, we newly include the extension of SiO layers as a precursor of silicate dust.

Influence of detailed in-depth radiation modeling on the computational predictions of liquid pool burning rates

Since thermal radiation substantially contributes to the flame heat feedback, a significant impact is anticipated for the in-depth radiation absorption in pool fires. This research focuses on investigating the influence of a detailed in-depth radiation absorption model on the accurate prediction of the flammability characteristics (i.e., ignition time and burning rate) of liquids in using computational fluid dynamics. First, we determined the radiative properties of hydrogenated tetrapropylene (TPH) (i.e., fuel used in the OECD PRISME project) using UV–Vis–NIR and FTIR spectroscopy and derived an expression for the depth-dependent absorption coefficient and average surface reflectivity. Then, a new approach was introduced for the modeling of in-depth radiation absorption. Subsequently, simulations were conducted for three test cases: heptane evaporation, pool fire, and spill fire scenarios involving both heptane and TPH. Results indicated mild effects of in-depth absorption modeling on heptane evaporation, negligible changes in heptane pool fires, and significant alterations in spill fires compared to the predictions with gray calculations. For all the studied cases except heptane pool fire, the ignition times decreased significantly. Sensitivity analysis revealed that the assumed source temperature had negligible influence on the mass loss rate predictions. The importance of the liquid’s Nusselt number (Nul) calculation varied between the studied scenarios.

Brief communication: Recent estimates of glacier mass loss for western North America from laser altimetry

Abstract. Glaciers in western North American outside of Alaska are often overlooked in global studies because their potential to contribute to changes in sea level is small. Nonetheless, these glaciers represent important sources of freshwater, especially during times of drought. Differencing recent ICESat-2 data from a digital elevation model derived from a combination of synthetic aperture radar data (TerraSAR-X/TanDEM-X), we find that over the period 2013–2020, glaciers in western North America lost mass at a rate of -12.3±3.5 Gt yr−1. This rate is comparable to the rate of mass loss (-11.7±1.0 Gt yr−1) for the period 2018–2022 calculated through trend analysis using ICESat-2 and Global Ecosystems Dynamics Investigation (GEDI) data.

Under Sulfate Dry–Wet Cycling: Exploring the Symmetry of the Mechanical Performance Trend and Grey Prediction of Lightweight Aggregate Concrete with Silica Powder Content

In order to improve the mechanical properties and durability of lightweight aggregate concrete in extreme environments, this study utilized Inner Mongolia pumice as the coarse aggregate to formulate pumice lightweight aggregate concrete (P-LWAC) with a silica powder content of 0%, 2%, 4%, 6%, 8%, and 10%. Under sulfate dry–wet cycling conditions, this study mainly conducted a mass loss rate test, compressive strength test, NMR test, and SEM test to investigate the improvement effect of silica powder content on the corrosion resistance performance of P-LWAC. In addition, using grey prediction theory, the relationship between pore characteristic parameters and compressive strength was elucidated, and a grey prediction model GM (1,3) was established to predict the compressive strength of P-LWAC after cycling. Research indicates that under sulfate corrosion conditions, as the cycle times and silica powder content increased, the corrosion resistance of P-LWAC showed a trend of first increasing and then decreasing. At 60 cycles, P-LWAC with a content of 6% exhibited the lowest mass loss rate and the highest relative dynamic elastic modulus, compressive strength, and corrosion resistance coefficient. From the perspective of data distribution, various durability indicators showed a clear mirror symmetry towards both sides with a silica powder content of 6% as the symmetrical center. The addition of silica fume reduced the porosity and permeability of P-LWAC, enhanced the saturation degree of bound fluid, and facilitated internal structural development from harmful pores towards less harmful and harmless pores, a feature most prominent at the 6% silica fume mixing ratio. In addition, a bound fluid saturation and pore size of 0.02~0.05 μm/% exerted the most significant influence on the compressive strength of P-LWAC subjected to 90 dry–wet cycles. Based on these two factors, grey prediction model GM (1,3) was established. This model can accurately evaluate the durability of P-LWAC, improving the efficiency of curing decision-making and construction of concrete materials.

The Optically Thick Rotating Magnetic Wind from a Massive White Dwarf Merger Product. II. Axisymmetric Magnetohydrodynamic Simulations

We numerically construct a series of axisymmetric rotating magnetic wind solutions, aiming at exploring the observation properties of massive white dwarf (WD) merger remnants with a strong magnetic field, a fast spin, and an intense mass loss, as inferred for WD J005311. We investigate the magnetospheric structure and the resultant spin-down torque exerted to the merger remnant with respect to the surface magnetic flux Φ*, spin angular frequency Ω* and the mass-loss rate Ṁ . We confirm that the wind properties for σ≡Φ*2Ω*2/Ṁvesc3≳1 significantly deviate from those of the spherical Parker wind, where v esc is the escape velocity at stellar surface. For such a rotating magnetic wind sequence, we find (i) a quasiperiodic mass eruption triggered by magnetic reconnection along with the equatorial plane and (ii) a scaling relation for the spin-down torque T≈(1/2)×ṀΩ*R*2σ1/4 . We apply our results to discuss the spin-down evolution and wind anisotropy of massive WD merger remnants, the latter of which could be probed by a successive observation of WD J005311 using Chandra.

Construction Strategy and Mechanism of a Novel Wood Preservative with Excellent Antifungal Effects.

Wood is a naturally porous material prone to microbial erosion and degradation in outdoor environments. Therefore, the development of an environmentally friendly wood preservative with excellent antibacterial effects and low toxicity is urgently needed. In this study, nitrogen-doped carbon quantum dots (N-CQDs) with excellent antifungal performance and fluorescent properties were synthesized using a one-step hydrothermal method with chitosan quaternary ammonium salt (HACC) as the raw material. The fluorescence characteristics of N-CQD preservatives can help track their position and distribution in wood. The minimum inhibitory concentration (MIC) of N-CQDs is 1.8 mg/mL, which was nearly 22 times lower than that of HACC (40.0 mg/mL) in the PDA medium. The decay resistance test demonstrated that wood treated with N-CQDs showed a considerably reduced decay degree and its mass loss rate decreased from 46 ± 0.5% to 3.8 ± 0.5%. Biological transmission electron microscopy revealed that N-CQDs effectively destroyed fungal cell structures, thereby hindering the growth of Coriolus versicolor. N-CQDs synthesized using the one-step hydrothermal method can be used as an efficient wood preservative that can effectively improve the utilization and service life of wood.

Interacting supernovae from wide massive binary systems

The features in the light curves and spectra of many I and II supernovae (SNe) can be understood by assuming an interaction of the SN ejecta with circumstellar matter (CSM) surrounding the progenitor star. This suggests that many massive stars may undergo various degrees of envelope stripping shortly before exploding, and may therefore produce a considerable diversity in their pre-explosion CSM properties. We explore a generic set of about 100 detailed massive binary evolution models in order to characterize the amount of envelope stripping and the expected CSM configurations. Our binary models were computed with the MESA stellar evolution code, considering an initial primary star mass of 12.6mso and secondaries with initial masses of between $ and $ and focus on initial orbital periods above $ We compute these models up to the time of iron core collapse in the primary. Our models exhibit varying degrees of stripping due to mass transfer, resulting in SN progenitor models ranging from fully stripped helium stars to stars that have not been stripped at all. We find that Roche lobe overflow often leads to incomplete stripping of the mass donor, resulting in a large variety of pre-SN envelope masses. In many of our models, the red supergiant (RSG) donor stars undergo core collapse during Roche lobe overflow, with mass transfer and therefore system mass-loss rates of up to $0.01 at that time. The corresponding CSM densities are similar to those inferred for IIn SNe, such as 1998S . In other cases, the mass transfer becomes unstable, leading to a common-envelope phase at such late time that the mass donor explodes before the common envelope is fully ejected or the system has merged. We argue that this may cause significant pre-SN variability, as witnessed for example in 2020tlf . Other models suggest a common-envelope ejection just centuries before core collapse, which may lead to the strongest interactions, as observed in superluminous IIn SNe, such as 1994W and 2006gy Wide massive binaries exhibit properties that may not only explain the diverse envelope stripping inferred in Type Ib, IIb, IIL, and IIP SNe, but also offer a natural framework to understand a broad range of hydrogen-rich interacting SNe. On the other hand, the flash features observed in many IIP SNe, such as 2013fs may indicate that RSG atmospheres are more extended than currently assumed; this could enhance the parameter space for wide binary interaction.

Insight into the evolution of membrane chemical degradation in proton exchange membrane fuel cells:From theoretical analysis to model developing

The chemical degradation of the proton exchange membrane (PEM) causes the changes in membrane properties and morphology, which directly affects the cell performance and membrane degradation. In this work, the changes of PEM during the chemical degradation are theoretically analyzed at both microscopic and mesoscopic levels. Based on the theoretical study, a bidirectionally coupled physical model of PEM fuel cell (PEMFC) performance and PEM chemical degradation is developed, which is used to investigate the evolutions of cell performance and chemical degradation. It can be found that the open circuit voltage first increases slightly and then decreases with time, and the ohmic loss increases rapidly under accelerated degradation conditions. The membrane chemical degradation is analyzed in terms of four aspects: the mass loss rate of the membrane, the region of pronounced degradation, the contribution of different degradation mechanisms and the proportion of ionomer species remaining. Furthermore, the effect of operating conditions on the degradation is examined. The degradation is most sensitive to voltage and has the fastest rate at high voltage, high temperature, high gas pressure and relative humidity of 60%. This work provides a deep insight into the PEM chemical degradation, which is instructive for the long-term prediction of PEMFC lifetime.

Mechanical characterization and water stability of loess improved by bio-based materials: An eco-friendly approach

Loess exhibits poor engineering properties, such as low strength and poor water stability. Conventional materials used for improving loess, such as cement and lime, result in environmental pollution issues throughout their production and application processes. To assess the efficacy of bio-based materials, including calcium alginate (CA), xanthan gum (XA), cotton fibers (CO) and flax fibers (FA) in the treatment of loess, the improved soil's strength, disintegration, and water resistance were examined. Subsequently, an optimal amendment approach was determined, and dry-wet cycle tests and microscopic observation were performed. The results show that 1.0 % calcium alginate can effectively enhance the strength of loess, significantly improving its resistance to disintegration with almost no observable disintegration; permeability is significantly reduced, and water repellency is enhanced. 2.0 % xanthan can improve the strength and disintegration resistance of loess, but the improvement in strength is lower than that of calcium alginate. Additionally, the improved soil with XA experiences a flocculent disintegration in static water, which cannot maintain the soil structure. Cotton fibers and flax fibers can enhance both compressive and tensile strength of the soil. The content of 0.45 % flax fibers is considered the optimal choice as it has no effect on water stability. Combining the above results, the combination of 1.0 % CA and 0.45 % FA has been selected to improve the loess, which effectively improves the comprehensive mechanical properties and water stability of the composite improved soil. The decrease in strength and mass loss rate are significantly reduced after dry-wet cycle tests. Microscopic tests show that calcium alginate connects soil particles by Ca2+ ionic bridges, which allows the cementing materials to fill the loess pores and exert the role of agglomeration and coagulation to enhance the integrity of the loess. This study shows that the bio-based material with calcium alginate as the main body can effectively improve the mechanical strength and water stability of the loess.

Corrosion characteristics of basalt-polypropylene hybrid fiber concrete under the compound salt and drying-wetting cycles

Concrete is widely used in civil engineering due to its superior properties, however, due to its crack-prone nature, its application in marine engineering will generate a large number of micro-cracks, which will affect the durability and service life of the concrete structure. Basalt-polypropylene hybrid fibers have been added to concrete as a new type of hybrid fiber to improve tensile strength. However, the long-term erosion resistance of basalt-polypropylene hybrid fiber concrete (BPHFC) in marine tidal environments has not been well studied. Therefore, the corrosion degradation behavior of BPHFC under the combined action of compound salt (NaCl+Na2SO4) and drying-wetting cycles was investigated using indoor simulation experiments, and analyzed the effects of fiber content and form on the macroscopic properties and sulfate concentration of concrete. In addition, the corrosion deterioration mechanism of BPHFC was revealed using a concrete surface pore structure analyzer, X-ray diffractometer, and field emission scanning electron microscopy. The research results showed that after 60 cycles, the mass loss rate of BPHFC began to increase, and the specimens mixed with 0.1% BF exhibited the smallest mass loss rate. The relative compressive strength (Kn) and relative dynamic elastic modulus showed a tendency to increase and then decrease. Compared with the control specimens, the addition of 0.1% BF, PF, or BF-PF reduced the Kn loss rate of concrete by 24.04%, 13.28%, and 8.10%, respectively, whereas 0.2% BF-PF hybrid fibers increased the Kn loss rate of concrete by 1.62%. The sulfate concentration of BPHFC increased with the number of cycles, and the addition of 0.1% single or hybrid fibers increased the magnitude of the decrease in sulfate concentration during the later stages of erosion. The addition of BF, PF, or hybrid BF-PF reduced the percentage of super-large pores in concrete by 0.67–28.91% after 90 cycles, and addition of BF and PF attenuated the deterioration of concrete pores after erosion. There was a difference in the bonding properties of BF and PF with the concrete matrix, and the corrosion products of BPHFC were mainly ettringite and gypsum. The results of this study contribute to the development and application of BPHFC in marine engineering.

Influence of corrosion on loading capacity of circular concrete-filled steel tubular column

Concrete-filled steel tubular (CFST) columns are commonly used in engineering, especially in load-bearing structures. This study conducts an in-depth examination of how the axial resistance of CFST columns varies with random corrosion. A finite element model for circular CFST columns is developed and its accuracy is verified using available experimental data. The interaction between the outer steel tube and the concrete column is explored, along with the introduction of a strength reduction coefficient concept. Additionally, the concept of an axial load-bearing capacity reduction coefficient is introduced to illustrate variations in the axial resistance of circular CFST columns during different corrosion stages. The degradation patterns of reduction coefficients for uniform and random corrosion depths in the steel tube and CFST columns with varying mass loss rates are analyzed, and formulas are provided to predict the axial resistance in different corrosion stages. Furthermore, the study investigates the influence of variables such as material strength, component dimensions, and the thickness of the external steel tube, resulting in adjustments to the original expressions for various conditions.

Study on experiments and numerical simulation of coal combustion characteristics under different thermal environments

In order to study heat release rate and flue gas generation during residual coal in goaf combustion, a cone calorimeter was used to research on combustion characteristics of bituminous coal under different heat radiation flux conditions. A novel coal fire FOAM solver for coal combustion is developed, numerically simulated by varying the gas atmosphere, and compared with the above experimental results. The results showed that with the increase in heat radiation flux, the shorter the time to reach the peak heat release rate, the greater the maximum heat release rate. When the coal does not enter the ignition stage, the CO production rate is higher than that after ignition, and the CO2 production rate is lower than that after ignition. Compared with the experimental results of the cone calorimeter, the difference between the two results is very small, which verified the feasibility and accuracy of the coal combustion model. After the injection of the composite inert gas, the heat release rate and mass loss rate of coal combustion have varying degrees of lag. The numerical simulation results can provide a theoretical basis for injecting inert compounds into the goaves of coal mines to prevent the spontaneous combustion of coal.

Under the light of a new star: evolution of planetary atmospheres through protoplanetary disc dispersal and boil-off

ABSTRACT The atmospheres of small, close-in exoplanets are vulnerable to rapid mass loss during protoplanetary disc dispersal via a process referred to as ‘boil-off’, in which confining pressure from the local gas disc reduces, inducing atmospheric loss and contraction. We construct self-consistent models of planet evolution during gaseous core accretion and boil-off. As the surrounding disc gas dissipates, we find that planets lose mass via subsonic breeze outflows which allow causal contact to exist between disc and planet. Planets initially accrete of order $\sim 10~{{\ \rm per\ cent}}$ in atmospheric mass, however, boil-off can remove $\gtrsim 90~{{\ \rm per\ cent}}$ of this mass during disc dispersal. We show that a planet’s final atmospheric mass fraction is strongly dictated by the ratio of cooling time-scale to disc dispersal time-scale, as well as the planet’s core mass and equilibrium temperature. With contributions from core cooling and radioactivity, we show that core luminosity eventually leads to the transition from boil-off to core-powered mass loss. We find that smaller mass planets closest to their host star may have their atmospheres completely stripped through a combination of boil-off and core-powered mass loss during disc dispersal, implying the existence of a population-level radius gap emerging as the disc disperses. We additionally consider the transition from boil-off/core-powered mass loss to X-ray and extreme ultraviolet (XUV) photoevaporation by considering the penetration of stellar XUV photons below the planet’s sonic surface. Finally, we show that planets may open gaps in their protoplanetary discs during the late stages of boil-off, which may enhance mass-loss rates.

Observed epochal variations in X-ray lines from the O supergiant ζ Puppis do not require substantial changes in the wind mass flux

ABSTRACT We fit the high-resolution Chandra X-ray spectra of the O supergiant ζ Puppis using the variable boundary condition (VBC) line model to test the stability of its mass-loss rate between two epochs of observation: 2000 March and 2018 July – 2019 August. At issue is whether the observed variations are induced by global changes in the cool (unshocked) wind itself or are isolated to the local pockets of hot gas (i.e. changes in the frequency and location of the shocks). Evidence in the literature favoured the possibility of a 40 per cent increase in the mass flux of the entire stellar wind, based on X-ray reabsorption from a line-deshadowing-instability-inspired parametrization, whereas our fit parameters are consistent with a constant mass flux with a change in the velocity variations that determine the locations where shocks form. Our results suggest the shocks in the more recent data are formed at somewhat larger radii, mimicking the enhanced blueshifts and increased line fluxes interpreted in the previous analysis as being due to increases in both the X-ray generation and reabsorption from an overall stronger wind.