Institut für Physik und Astronomie
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Stars are the most fundamental constituents of galaxies. The age, distribution, and composition of the stars in a galaxy can be used to derive the history and evolution of the host galaxy. The stars are responsible for synthesizing and distributing heavier elements. The understanding of the host stars is essential to decode the characteristics of planetary systems. This means that studying the formation, evolution, and death of stars is a central field of astrophysics.
Most stars are not born alone but are found to have one or several companions. In a significant fraction of those systems, the companions will interact with each other during their lifetime and so influence each other significantly. This can lead to substantial changes in the evolution of stars in close binary systems and cannot be neglected, if we want to understand stellar evolution. There are different kinds of interactions, which are observed. Tidal interactions can influence the stellar rotation velocity. Strong irradiation can alter the structure of the companions and is vital also for the understanding of close-in planets such as Hot Jupiters. Magnetic interactions can change the orbital period of the binary systems.
The most important interaction is mass transfer from one star to the other. Depending on the initial separation of the system, this can happen in different evolutionary phases. The mass ratio of both stars in the binary system is determining, if the mass transfer is stable or not. Binary systems with two stars of similar mass can experience stable mass transfer when they are close enough. Thereby mass is transferred from one star to the other, changing both stellar masses. The companion accreting the matter is spun-up and so rejuvenated. In systems where the stars have significantly different masses, the mass transfer is expected to happen on a dynamical timescale and the rate of mass transfer will be so high that a common envelope around both stars is formed. Friction in the envelope leads to a rapid shrinking of the orbit on the timescale of a few thousands of days and is difficult to observe. The observation of many evolved systems with orbital separations smaller than the radius of a red giant shows that such a phase must exist. During the spiral-in, energy and angular momentum is transferred to the envelope and can lead to its ejection, when the transferred energy is sufficient to unbind it.
Common-envelope evolution is crucial to understand many exciting systems, which are ob- served in our universe. It is essential for the formation of stellar-mass gravitational merger sources, as it can bring compact-object binaries close enough together so that gravitational waves can lead to a merger within a Hubble time. This phase is also vital for the understanding of progenitor systems of supernovae type Ia, which are used as standard candles to derive distances to far galaxies. With their help the existence of cosmological dark energy could be inferred. Supernovae type Ia are thought to be produced by the explosion of carbon-oxygen white dwarfs exceeding their upper mass limit, the Chandrasekhar mass. The most likely progenitor systems are still under debate.
The common envelope phase is one of the most significant and least-constrained processes in stellar binary evolution, and one of the most important unsolved problems in the understanding of stellar evolution. As it is a short-lived phase, direct observations are very unlikely and a statistically significant sample of systems after this phase is necessary to gain insight into it. For the physical understanding of this process (magneto-) hydrodynamical simulations have to be performed. A large enough sample of post-common envelope systems with observed masses, radii and orbital separations can provide the parameter range that has to be explained by the simulations.
In this thesis, I make a significant contribution to the investigation of binary systems after the common envelope phase by newly discovering a large sample post-common envelope systems and also significantly increasing the number of systems with derived parameters. This sample is a first step to acquire a statistically significant sample for a better understanding of this crucial but not yet understood phase. Moreover, I also present the detailed analysis of several kinds of interesting close binary systems studying different aspects of these systems, as the influence of tidal forces, the effect of mass transfer and orbital period changes among other things.
I will give a short introduction to the current state of knowledge regarding stellar evolution of single stars and the influence of close companions on this evolution. Moreover, I give a short introduction into the different kinds of close binary systems we studied. I also give a short summary of the methods used to investigate those systems. Subsequently, to the appended papers, I will discuss the results and give a short summary.
The study initiates with the properties of triple cation pin solar cells as a function of their changing bandgap. The standard device layout comprises PTAA as hole-transport layer (HTL) and C60/BCP as electron-transport layer (ETL). The bandgap of the composition Cs0.05(FAxMA1-x)0.95Pb(IxBr1-x)3 can be linearly changed from 1.52 eV (x=1) to 1.88 eV (x=0.5). However, the VOC of the devices plateaus around 1.17 V instead of increasing as theoretically expected. Although these VOC losses were traditionally ascribed to halide segregation, we quantified the radiative efficiency losses of the devices by measuring the electroluminescence quantum efficiency Qlume as a function of the bromine content. The VOC calculated from Qlume matches the VOC of the J-V measurements in all the cases, concluding that non-radiative recombination losses are directly proportional to the bromine content, hence the VOC pinning. Non-radiative losses can be partially mitigated by the addition of LiF as a passivation layer before the ETL until the bandgap reaches 1.74 eV. Above this value, both the n and p interfaces require further optimisation to increase the VOC. Changing the HTL to 2PACz, adding oleylamine to the precursor solution and LiF as a passivation agent before the C60, accomplish altogether a stepwise reduction in the non-radiative losses attaining finally 83% of the radiative limit for the open-circuit voltage (VOC,rad) in cells with bandgaps of 1.80, 1.85 and 1.88 eV. Subsequently, we fabricated monolithic 2-terminal tandem solar cells with a Pb-Sn perovskite as the low-bandgap subcell and a recombination layer of AZO/SnOx/InOx. We attempted the three already-optimised aforementioned bandgaps (1.80, 1.85 and 1.88 eV) for the top high-bandgap subcell. The best combination was found to be 1.85/1.27 eV reaching 23.7% stabilised power output. Further analysis included subcell characterisation by (injection dependent) electro- and (intensity dependent) photoluminescence to assess both the implied efficiency potential and the limitations. Transport losses seen in the FF reduce the performance of the tandem from its efficiency potential of 25.2%. The low external quantum efficiency seen in the low-bandgap standard subcell is explained but its non-optimal absorption, an issue that is solved by increasing the thickness of the active layer, boosting in that way the efficiency up to 25.9% in a proof-of-concept device with a 30% of implied efficiency. In order to gain insights in the device physics, we investigated several perovskite compositions to quantify the electronic doping and its impact on device performance. Using AC Hall effect, this doping density is of the order of 1e11-1e13 cm-3 in Pb-based perovskites. By observing how the recombination regimes change upon the light intensity in photoluminescence quantum yield and transient photoluminescence measurements, it was found that Sn-based perovskites exhibit a higher doping concentration (1e14 cm-3) in comparison to Pb-based ones (1e12 cm-3). By using charge-extraction techniques, the electrode charge per cell volume under short-circuit conditions (1e16 cm-3), was found to be much higher than the presumable doping density, concluding (supported by simulations) that the latter does not affect the device performance. However, at longer time scales (ms-s) much larger charge concentrations were detected. We concluded that the changes in the internal electrostatic field do not come from doping but from these concentration of mobile ions that amount to roughly 1e17 cm-3 in fresh devices. This ionic concentration can be assessed and accurately quantified by bias-assisted charge extraction (BACE) and by measuring the J-V scans of the cells at different scan rates. At high scan speeds, the ions do not react to the changing field and therefore, neither field screening nor hysteresis are observed. At low scan speeds, hysteresis is not present either, yet the ions have enough time to go back to interface where they screen the internal field the most. In the points in between, both hysteresis and field screening manifest depending on the scan rate. The accuracy of charge extraction under linearly increasing voltage (CELIV) in comparison to BACE when it comes to the determination of the ionic density is lower owing to the initial ionic distribution at short-circuit condition. Mott-Schottky analysis at low frequency was performed in order to complement BACE in the estimation of the ionic density, which result in a value of 2.4e17 cm-3, which rises to 7.5e17 cm-3 after 5 hours under 1 sun equivalent illumination and open-circuit conditions.
Galaxy morphology is a fossil record of how galaxies formed and evolved and can be regarded as a function of the dynamical state of a galaxy. It encodes the physical processes that dominate its evolutionary history, and is strongly aligned with physical properties like stellar mass, star formation rate and local environment. At a distance of ∼50 and 60 kpc, the Magellanic Clouds represent the nearest interacting pair of dwarf irregular galaxies to the Milky Way, rendering them an important test bed for galaxy morphology in the context of galaxy interactions and the effect of the local environment in which they reside. The Large Magellanic Cloud is classified as the prototype for Magellanic Spiral galaxies, with one prominent spiral arm, an offset bar and an inclined rotating disc while the Small Magellanic Cloud is classified as a dwarf Irregular galaxy and is known for its unstructured shape and large depth across the line–of–sight. Resolved stellar populations are powerful probes of a wide range of astrophysical phenomena, the proximity of the Magellanic Clouds allows us to resolve their stellar populations to individual stars that share coherent chemical and age distributions. The coherent properties of resolved stellar populations enable us to analyse them as a function of position within the Magellanic Clouds, offering a picture of the growth of the galaxies’ substructures over time and yielding a comprehensive view of their morphology. Furthermore, investigating the kinematics of the Magellanic Clouds offers valuable insights into their dynamics and evolutionary history. By studying the motions and velocities of stars within these galaxies, we can trace their past interactions, with the Milky Way or with each other and unravel the complex interplay of forces that have influenced the Magellanic Clouds’ formation and evolution.
In Chapter 2, the VISTA survey of the Magellanic Clouds was employed to generate unprecedented high-resolution morphological maps of the Magellanic Clouds in the near-infrared. Utilising colour-magnitude diagrams and theoretical evolutionary models to segregate stellar populations, this approach enabled a comprehensive age tomography of the galaxies. It revealed previously uncharacterised features in their central regions at spatial resolutions of 0.13 kpc (Large Magellanic Cloud) and 0.16 kpc (Small Magellanic Cloud), the findings showcased the impact of tidal interactions on their inner regions. Notably, the study highlighted the enhanced coherent structures in the Large Magellanic Cloud, shedding light on the significant role of the recent Magellanic Clouds’ interaction 200 Myr ago in shaping many of the fine structures. The Small Magellanic Cloud revealed asymmetry in younger populations and irregularities in intermediate-age ones, pointing towards the influence of past tidal interactions.
In Chapter 3, an examination of the outskirts of the Magellanic Clouds led to the identification of new substructures through the use of near-infrared photometry from the VISTA Hemisphere Survey and multi-dimensional phase-space information from Gaia. The distances and proper motions of these substructures were investigated. This analysis revealed the impact of past Magellanic Clouds’ interactions and the influence of the Milky Way’s tidal field on the morphology and kinematics of the Magellanic Clouds. A bi-modal distance distribution was identified within the luminosity function of the red clump stars in the Small Magellanic Cloud, notably in its eastern regions, with the foreground substructure being attributed to the Magellanic Clouds’ interaction around 200 Myr ago. Furthermore, associations with the Counter Bridge and Old Bridge were uncovered through the detection of background and foreground structures in various regions of the SMC.
In chapter 4, a detailed kinematic analysis of the Small Magellanic Cloud was conducted using spectra from the European Southern Observatory Science Archive Facility. The study reveals distinct kinematics in the Wing and bar regions, attributed to interactions with the Large Magellanic Cloud and variations in star formation history. Notably, velocity disparities are observed in the bar’s young main sequence stars, aligning with specific star-forming episodes, and suggesting potential galactic stretching or tidal stripping, as corroborated by proper motion studies.
On the effects of disorder on the ability of oscillatory or directional dynamics to synchronize
(2024)
In this thesis I present a collection of publications of my work, containing analytic results and observations in numerical experiments on the effects of various inhomogeneities, on the ability of coupled oscillators to synchronize their collective dynamics. Most of these works are concerned with the effects of Gaussian and non-Gaussian noise acting on the phase of autonomous oscillators (Secs. 2.1-2.4) or on the direction of higher dimensional state vectors (Secs. 2.5,2.6). I obtain exact and approximate solutions to the non-linear equations governing the distributions of phases, or perform linear stability analysis of the uniform distribution to obtain the transition point from a completely disordered state to partial order or more complicated collective behavior. Other inhomogeneities, that can affect synchronization of coupled oscillators, are irregular, chaotic oscillations or a complex, and possibly random structure in the coupling network. In Section 2.9 I present a new method to define the phase- and frequency linear response function for chaotic oscillators. In Sections 2.4, 2.7 and 2.8 I study synchronization in complex networks of coupled oscillators. Each section in Chapter 2 - Manuscripts, is devoted to one research paper and begins with a list of the main results, a description of my contributions to the work and a short account of the scientific context, i.e. the questions and challenges which started the research and the relation of the work to my other research projects. The manuscripts in this thesis are reproductions of the arXiv versions, i.e. preprints under the creative commons licence.
Massive stars (Mini > 8 Msol) are the key feedback agents within galaxies, as they shape their surroundings via their powerful winds, ionizing radiation, and explosive supernovae. Most massive stars are born in binary systems, where interactions with their companions significantly alter their evolution and the feedback they deposit in their host galaxy. Understanding binary evolution, particularly in the low-metallicity environments as proxies for the Early Universe, is crucial for interpreting the rest-frame ultraviolet spectra observed in high-redshift galaxies by telescopes like Hubble and James Webb.
This thesis aims to tackle this challenge by investigating in detail massive binaries within the low-metallicity environment of the Small Magellanic Cloud galaxy. From ultraviolet and multi-epoch optical spectroscopic data, we uncovered post-interaction binaries. To comprehensively characterize these binary systems, their stellar winds, and orbital parameters, we use a multifaceted approach. The Potsdam Wolf-Rayet stellar atmosphere code is employed to obtain the stellar and wind parameters of the stars. Additionally, we perform consistent light and radial velocity fitting with the Physics of Eclipsing Binaries software, allowing for the independent determination of orbital parameters and component masses. Finally, we utilize these results to challenge the standard picture of stellar evolution and improve our understanding of low-metallicity stellar populations by calculating our binary evolution models with the Modules for Experiments in Stellar Astrophysics code.
We discovered the first four O-type post-interaction binaries in the SMC (Chapters 2, 5, and 6). Their primary stars have temperatures similar to other OB stars and reside far from the helium zero-age main sequence, challenging the traditional view of binary evolution. Our stellar evolution models suggest this may be due to enhanced mixing after core-hydrogen burning. Furthermore, we discovered the so-far most massive binary system undergoing mass transfer (Chapter 3), offering a unique opportunity to test mass-transfer efficiency in extreme conditions. Our binary evolution calculations revealed unexpected evolutionary pathways for accreting stars in binaries, potentially providing the missing link to understanding the observed Wolf-Rayet population within the SMC (Chapter 4). The results presented in this thesis unveiled the properties of massive binaries at low-metallicity which challenge the way the spectra of high-redshift galaxies are currently being analyzed as well as our understanding of massive-star feedback within galaxies.
Astrophysical shocks, driven by explosive events such as supernovae, efficiently accelerate charged particles to relativistic energies. The majority of these shocks occur in collisionless plasmas where the energy transfer is dominated by particle-wave interactions.Strong nonrelativistic shocks found in supernova remnants are plausible sites of galactic cosmic ray production, and the observed emission indicates the presence of nonthermal electrons. To participate in the primary mechanism of energy gain - Diffusive Shock Acceleration - electrons must have a highly suprathermal energy, implying a need for very efficient pre-acceleration. This poorly understood aspect of the shock acceleration theory is known as the electron injection problem. Studying electron-scale phenomena requires the use of fully kinetic particle-in-cell (PIC) simulations, which describe collisionless plasma from first principles.
Most published studies consider a homogenous upstream medium, but turbulence is ubiquitous in astrophysical environments and is typically driven at magnetohydrodynamic scales, cascading down to kinetic scales. For the first time, I investigate how preexisting turbulence affects electron acceleration at nonrelativistic shocks using the fully kinetic approach. To accomplish this, I developed a novel simulation framework that allows the study of shocks propagating in turbulent media. It involves simulating slabs of turbulent plasma separately, which are further continuously inserted into a shock simulation. This demands matching of the plasma slabs at the interface. A new procedure of matching electromagnetic fields and currents prevents numerical transients, and the plasma evolves self-consistently. The versatility of this framework has the potential to render simulations more consistent with turbulent systems in various astrophysical environments.
In this Thesis, I present the results of 2D3V PIC simulations of high-Mach-number nonrelativistic shocks with preexisting compressive turbulence in an electron-ion plasma. The chosen amplitudes of the density fluctuations ($\lesssim15\%$) concord with \textit{in situ} measurements in the heliosphere and the local interstellar medium. I explored how these fluctuations impact the dynamics of upstream electrons, the driving of the plasma instabilities, electron heating and acceleration. My results indicate that while the presence of the turbulence enhances variations in the upstream magnetic field, their levels remain too low to influence the behavior of electrons at perpendicular shocks significantly. However, the situation is different at oblique shocks. The external magnetic field inclined at an angle between $50^\circ \lesssim \theta_\text{Bn} \lesssim 75^\circ$ relative to the shock normal allows the escape of fast electrons toward the upstream region. An extended electron foreshock region is formed, where these particles drive various instabilities. Results of an oblique shock with $\theta_\text{Bn}=60^\circ$ propagating in preexisting compressive turbulence show that the foreshock becomes significantly shorter, and the shock-reflected electrons have higher temperatures. Furthermore, the energy spectrum of downstream electrons shows a well-pronounced nonthermal tail that follows a power law with an index up to -2.3.
The methods and results presented in this Thesis could serve as a starting point for more realistic modeling of interactions between shocks and turbulence in plasmas from first principles.
Condensation and crystallization are omnipresent phenomena in nature. The formation of droplets or crystals on a solid surface are familiar processes which, beyond their scientific interest, are required in many technological applications. In recent years, experimental techniques have been developed which allow patterning a substrate with surface domains of molecular thickness, surface area in the mesoscopic scale, and different wettabilities (i.e., different degrees of preference for a substance that is in contact with the substrate). The existence of new patterned surfaces has led to increased theoretical efforts to understand wetting phenomena in such systems.
In this thesis, we deal with some problems related to the equilibrium of phases (e.g., liquid-vapor coexistence) and the kinetics of phase separation in the presence of chemically patterned surfaces. Two different cases are considered: (i) patterned surfaces in contact with liquid and vapor, and (ii) patterned surfaces in contact with a crystalline phase. One of the problems that we have studied is the following: It is widely believed that if air containing water vapor is cooled to its dew point, droplets of water are immediately formed. Although common experience seems to support this view, it is not correct. It is only when air is cooled well below its dew point that the phase transition occurs immediately. A vapor cooled slightly below its dew point is in a metastable state, meaning that the liquid phase is more stable than the vapor, but the formation of droplets requires some time to occur, which can be very long.
It was first pointed out by J. W. Gibbs that the metastability of a vapor depends on the energy necessary to form a nucleus (a droplet of a critical size). Droplets smaller than the critical size will tend to disappear, while droplets larger than the critical size will tend to grow. This is consistent with an energy barrier that has its maximum at the critical size, as is the case for droplets formed directly in the vapor or in contact with a chemically uniform planar wall. Classical nucleation theory describes the time evolution of the condensation in terms of the random process of droplet growth through this energy barrier. This process is activated by thermal fluctuations, which eventually will form a droplet of the critical size.
We consider nucleation of droplets from a vapor on a substrate patterned with easily wettable (lyophilic) circular domains. Under certain conditions of pressure and temperature, the condensation of a droplet on a lyophilic circular domain proceeds through a barrier with two maxima (a double barrier). We have extended classical nucleation theory to account for the kinetics of nucleation through a double barrier, and applied this extension to nucleation on lyophilic circular domains.
Laser induced switching offers an attractive possibility to manipulate small magnetic domains for prospective memory and logic devices on ultrashort time scales. Moreover, optical control of magnetization without high applied magnetic fields allows manipulation of magnetic domains individually and locally, without expensive heat dissipation. One of the major challenges for developing novel optically controlled magnetic memory and logic devices is reliable formation and annihilation of non-volatile magnetic domains that can serve as memory bits in ambient conditions. Magnetic skyrmions, topologically nontrivial spin textures, have been studied intensively since their discovery due to their stability and scalability in potential spintronic devices. However, skyrmion formation and, especially, annihilation processes are still not completely understood and further investigation on such mechanisms are needed. The aim of this thesis is to contribute to better understanding of the physical processes behind the optical control of magnetism in thin films, with the goal of optimizing material parameters and methods for their potential use in next generation memory and logic devices.
First part of the thesis is dedicated to investigation of all-optical helicity-dependent switching (AO-HDS) as a method for magnetization manipulation. AO-HDS in Co/Pt multilayer and CoFeB alloys with and without the presence of Dzyaloshinskii-Moriya interaction (DMI), which is a type of exchange interaction, have been investigated by magnetic imaging using photo-emission electron microscopy (PEEM) in combination with X-ray magnetic circular dichroism (XMCD). The results show that in a narrow range of the laser fluence, circularly polarized laser light induces a drag on domain walls. This enables a local deterministic transformation of the magnetic domain pattern from stripes to bubbles in out-of-plane magnetized Co/Pt multilayers, only controlled by the helicity of ultrashort laser pulses. The temperature and characteristic fields at which the stripe-bubble transformation occurs has been calculated using theory for isolated magnetic bubbles, using as parameters experimentally determined average size of stripe domains and the magnetic layer thickness.
The second part of the work aims at purely optical formation and annihilation of magnetic skyrmions by a single laser pulse. The presence of a skyrmion phase in the investigated CoFeB alloys was first confirmed using a Kerr microscope. Then the helicity-dependent skyrmion manipulation was studied using AO-HDS at different laser fluences. It was found that formation or annihilation individual skyrmions using AO-HDS is possible, but not always reliable, as fluctuations in the laser fluence or position can easily overwrite the helicity-dependent effect of AO-HDS. However, the experimental results and magnetic simulations showed that the threshold values for the laser fluence for the formation and annihilation of skyrmions are different. A higher fluence is required for skyrmion formation, and existing skyrmions can be annihilated by pulses with a slightly lower fluence. This provides a further option for controlling formation and annihilation of skyrmions using the laser fluence. Micromagnetic simulations provide additional insights into the formation and annihilation mechanism.
The ability to manipulate the magnetic state of individual skyrmions is of fundamental importance for magnetic data storage technologies. Our results show for the first time that the optical formation and annihilation of skyrmions is possible without changing the external field. These results enable further investigations to optimise the magnetic layer to maximise the energy gap between the formation and annihilation barrier. As a result, unwanted switching due to small laser fluctuations can be avoided and fully deterministic optical switching can be achieved.
Arctic climate change is marked by intensified warming compared to global trends and a significant reduction in Arctic sea ice which can intricately influence mid-latitude atmospheric circulation through tropo- and stratospheric pathways. Achieving accurate simulations of current and future climate demands a realistic representation of Arctic climate processes in numerical climate models, which remains challenging.
Model deficiencies in replicating observed Arctic climate processes often arise due to inadequacies in representing turbulent boundary layer interactions that determine the interactions between the atmosphere, sea ice, and ocean. Many current climate models rely on parameterizations developed for mid-latitude conditions to handle Arctic turbulent boundary layer processes.
This thesis focuses on modified representation of the Arctic atmospheric processes and understanding their resulting impact on large-scale mid-latitude atmospheric circulation within climate models. The improved turbulence parameterizations, recently developed based on Arctic measurements, were implemented in the global atmospheric circulation model ECHAM6. This involved modifying the stability functions over sea ice and ocean for stable stratification and changing the roughness length over sea ice for all stratification conditions. Comprehensive analyses are conducted to assess the impacts of these modifications on ECHAM6's simulations of the Arctic boundary layer, overall atmospheric circulation, and the dynamical pathways between the Arctic and mid-latitudes.
Through a step-wise implementation of the mentioned parameterizations into ECHAM6, a series of sensitivity experiments revealed that the combined impacts of the reduced roughness length and the modified stability functions are non-linear. Nevertheless, it is evident that both modifications consistently lead to a general decrease in the heat transfer coefficient, being in close agreement with the observations.
Additionally, compared to the reference observations, the ECHAM6 model falls short in accurately representing unstable and strongly stable conditions.
The less frequent occurrence of strong stability restricts the influence of the modified stability functions by reducing the affected sample size. However, when focusing solely on the specific instances of a strongly stable atmosphere, the sensible heat flux approaches near-zero values, which is in line with the observations. Models employing commonly used surface turbulence parameterizations were shown to have difficulties replicating the near-zero sensible heat flux in strongly stable stratification.
I also found that these limited changes in surface layer turbulence parameterizations have a statistically significant impact on the temperature and wind patterns across multiple pressure levels, including the stratosphere, in both the Arctic and mid-latitudes. These significant signals vary in strength, extent, and direction depending on the specific month or year, indicating a strong reliance on the background state.
Furthermore, this research investigates how the modified surface turbulence parameterizations may influence the response of both stratospheric and tropospheric circulation to Arctic sea ice loss.
The most suitable parameterizations for accurately representing Arctic boundary layer turbulence were identified from the sensitivity experiments. Subsequently, the model's response to sea ice loss is evaluated through extended ECHAM6 simulations with different prescribed sea ice conditions.
The simulation with adjusted surface turbulence parameterizations better reproduced the observed Arctic tropospheric warming in vertical extent, demonstrating improved alignment with the reanalysis data. Additionally, unlike the control experiments, this simulation successfully reproduced specific circulation patterns linked to the stratospheric pathway for Arctic-mid-latitude linkages. Specifically, an increased occurrence of the Scandinavian-Ural blocking regime (negative phase of the North Atlantic Oscillation) in early (late) winter is observed. Overall, it can be inferred that improving turbulence parameterizations at the surface layer can improve the ECHAM6's response to sea ice loss.
Improving permafrost dynamics in land surface models: insights from dual sensitivity experiments
(2024)
The thawing of permafrost and the subsequent release of greenhouse gases constitute one of the most significant and uncertain positive feedback loops in the context of climate change, making predictions regarding changes in permafrost coverage of paramount importance. To address these critical questions, climate scientists have developed Land Surface Models (LSMs) that encompass a multitude of physical soil processes. This thesis is committed to advancing our understanding and refining precise representations of permafrost dynamics within LSMs, with a specific focus on the accurate modeling of heat fluxes, an essential component for simulating permafrost physics.
The first research question overviews fundamental model prerequisites for the representation of permafrost soils within land surface modeling. It includes a first-of-its-kind comparison between LSMs in CMIP6 to reveal their differences and shortcomings in key permafrost physics parameters. Overall, each of these LSMs represents a unique approach to simulating soil processes and their interactions with the climate system. Choosing the most appropriate model for a particular application depends on factors such as the spatial and temporal scale of the simulation, the specific research question, and available computational resources.
The second research question evaluates the performance of the state-of-the-art Community Land Model (CLM5) in simulating Arctic permafrost regions. Our approach overcomes traditional evaluation limitations by individually addressing depth, seasonality, and regional variations, providing a comprehensive assessment of permafrost and soil temperature dynamics. I compare CLM5's results with three extensive datasets: (1) soil temperatures from 295 borehole stations, (2) active layer thickness (ALT) data from the Circumpolar Active Layer Monitoring Network (CALM), and (3) soil temperatures, ALT, and permafrost extent from the ESA Climate Change Initiative (ESA-CCI). The results show that CLM5 aligns well with ESA-CCI and CALM for permafrost extent and ALT but reveals a significant global cold temperature bias, notably over Siberia. These results echo a persistent challenge identified in numerous studies: the existence of a systematic 'cold bias' in soil temperature over permafrost regions. To address this challenge, the following research questions propose dual sensitivity experiments.
The third research question represents the first study to apply a Plant Functional Type (PFT)-based approach to derive soil texture and soil organic matter (SOM), departing from the conventional use of coarse-resolution global data in LSMs. This novel method results in a more uniform distribution of soil organic matter density (OMD) across the domain, characterized by reduced OMD values in most regions. However, changes in soil texture exhibit a more intricate spatial pattern. Comparing the results to observations reveals a significant reduction in the cold bias observed in the control run. This method shows noticeable improvements in permafrost extent, but at the cost of an overestimation in ALT. These findings emphasize the model's high sensitivity to variations in soil texture and SOM content, highlighting the crucial role of soil composition in governing heat transfer processes and shaping the seasonal variation of soil temperatures in permafrost regions.
Expanding upon a site experiment conducted in Trail Valley Creek by \citet{dutch_impact_2022}, the fourth research question extends the application of the snow scheme proposed by \citet{sturm_thermal_1997} to cover the entire Arctic domain. By employing a snow scheme better suited to the snow density profile observed over permafrost regions, this thesis seeks to assess its influence on simulated soil temperatures. Comparing this method to observational datasets reveals a significant reduction in the cold bias that was present in the control run. In most regions, the Sturm run exhibits a substantial decrease in the cold bias. However, there is a distinctive overshoot with a warm bias observed in mountainous areas. The Sturm experiment effectively addressed the overestimation of permafrost extent in the control run, albeit resulting in a substantial reduction in permafrost extent over mountainous areas. ALT results remain relatively consistent compared to the control run. These outcomes align with our initial hypothesis, which anticipated that the reduced snow insulation in the Sturm run would lead to higher winter soil temperatures and a more accurate representation of permafrost physics.
In summary, this thesis demonstrates significant advancements in understanding permafrost dynamics and its integration into LSMs. It has meticulously unraveled the intricacies involved in the interplay between heat transfer, soil properties, and snow dynamics in permafrost regions. These insights offer novel perspectives on model representation and performance.