Beeinflussung der Grenzflächenspannung zwischen den Schmelzen "unverträglicher" Homopolymere durch Copolymere

Im Rahmen dieser Arbeit wurde am System Polyethylenoxid / Polypropylenoxid (PEO / PPO) der Einfluß von Copolymeren auf die Grenzflächenspannung Sigma von Homopolymerblends untersucht. Als Additive dienten Triblockcopolymere EO-block-PO-block-EO bzw. PO-block-EO-block-PO, Diblockcopolymere S-block-EO sowie statistische Copolymere EO-ran-PO. Die Additive wurden so ausgewählt, daß sich Paare von Additiven jeweils in genau einer Eigenschaft (Zusammensetzung, Kettenlänge, Blockanordnung) unterscheiden, in allen anderen Parametern jedoch vergleichbar sind. Die Grenzflächenspannung wurde experimentell mit Hilfe der Pendant-Drop-Methode in Abhängigkeit von der Temperatur ermittelt, wobei das Polymer mit der höheren Dichte, PEO, die Tropfenphase und PPO die Matrixphase bildet. Das Additiv wurde bei Messung der Grenzflächenspannung der ternären Systeme in unterschiedlichen Konzentrationen entweder einer oder beiden Homopolymerphasen zugegeben. Die Konzentrationsabhängigkeit von Sigma lässt sich sowohl mit dem Modell von Tang und Huang als auch mit einem Langmuir-analogen Ansatz gut beschreiben.Um den Zusammenhang zwischen sigma und dem Phasenverhalten zu untersuchen, wurden für einige der ternären Systeme Trübungskurven bei 100°C aufgenommen. Der Vergleich zwischen den Phasendiagrammen und den korrespondierenden Werten von sigma weist darauf hin, dass ein Additiv sigma gerade dann wirksam reduziert, wenn es einem Homopolymer zugefügt wird, mit dem es nur begrenzt verträglich ist, da dann die Triebkraft zur Anlagerung an der Grenzfläche besonders ausgeprägt ist. Das bereits bekannte Phänomen, wonach der Wert der Grenzflächenspannung davon abhängig sein kann, in welcher der Phasen das Additiv zu Beginn der Messung vorliegt, wurde ausführlich untersucht. Es wird angenommen, dass das System nicht in jedem Fall das thermodynamische Gleichgewicht erlangt und der beobachtete Effekt auf das Erreichen stationärer Zustände zurückzuführen ist. Dieses Verhalten kann mit einem Modell beschrieben werden, in welches das Viskositätsverhältnis der Homopolymere sowie der Verteilungskoeffizient des Copolymers zwischen den Homopolymerphasen eingehen. Aus Löslichkeitsparametern wurde der binäre Wechselwirkungsparameter Chi PEO/PPO = 0.18 abgeschätzt und mit diesem die theoretischen Werte für sigma zwischen PEO und PPO nach den Modellen von Roe bzw. Helfand und Tagami berechnet. Der Vergleich mit den experimentellen Daten des binären Systems zeigt, dass beide Ansätze sigma-Werte liefern, die in der Größenordnung der experimentellen Daten liegen, hierbei erweist sich der Ansatz von Roe als besonders geeignet. Die Temperaturabhängigkeit der Grenzflächenspannung wird jedoch durch beide Ansätze unzutreffend wiedergegeben. Mit dem Modell von Helfand und Tagami wurden eine Grenzflächendicke von 7.9 Å und das Dichteprofil der Grenzfläche berechnet. Für die Copolymere EO92PO56EO92 und S9EO22 (die Indices geben die Zahl der Monomereinheiten an) können die Grenzflächenüberschusskonzentrationen, die kritische Mizellenkonzentration sowie der einem Additivmolekül an der Grenzschicht zur Verfügung stehende Platz bestimmt werden.Der Vergleich unterschiedlicher Copolymere hinsichtlich ihrer Fähigkeit, sigma wirkungsvoll herabzusetzen, zeigt, dass im Fall von Triblockcopolymeren die Anordnung der Blöcke gegenüber der Zusammensetzung eine untergeordnete Rolle spielt. Mit zunehmender Kettenlänge nimmt die Effektivität als Compatibilizer sowohl bei Blockcopolymeren als auch bei statistischen Copolymeren zu.

Grazing incidence pumped Zr x-ray laser for spectroscopy on Li-like ions

X-ray laser fluorescence spectroscopy of the 2s-2p transition in Li-like ions is promising to become a widely applicable tool to provide information on the nuclear charge radii of stable and radioactive isotopes. For performing such experiments at the Experimental Storage Ring ESR, and the future NESR within the FAIR Project, a grazing incidence pumped (GRIP) x-ray laser (XRL) was set up at GSI Darmstadt using PHELIX (Petawatt High Energy Laser for heavy Ions eXperiments). The experiments demonstrated that lasing using the GRIP geometry could be achieved with relatively low pump energy, a prerequisite for higher repetition rate. In the first chapter the need of a plasma XRL is motivated and a short history of the plasma XRL is presented. The distinctive characteristic of the GRIP method is the controlled deposition of the pump laser energy into the desired plasma density region. While up to now the analysis performed were mostly concerned with the plasma density at the turning point of the main pump pulse, in this thesis it is demonstrated that also the energy deposition is significantly modified for the GRIP method, being sensitive in different ways to a large number of parameters. In the second chapter, the theoretical description of the plasma evolution, active medium and XRL emission properties are reviewed. In addition an innovative analysis of the laser absorption in plasma which includes an inverse Bremsstrahlung (IB) correction factor is presented. The third chapter gives an overview of the experimental set-up and diagnostics, providing an analytical formula for the average and instantaneous traveling wave speed generated with a tilted, on-axis spherical mirror, the only focusing system used up to now in GRIP XRL. The fourth chapter describes the experimental optimization and results. The emphasis is on the effect of the incidence angle of the main pump pulse on the absorption in plasma and on output and gain in different lasing lines. This is compared to the theoretical results for two different incidence angles. Significant corrections for the temperature evolution during the main pump pulse due to the incidence angle are demonstrated in comparison to a simple analytical model which does not take into account the pumping geometry. A much better agreement is reached by the model developed in this thesis. An interesting result is also the appearance of a central dip in the spatially resolved keV emission which was observed in the XRL experiments for the first time and correlates well with previous near field imaging and plasma density profile measurements. In the conclusion also an outlook to the generation of shorter wavelength XRL’s is given.

Eine kontinuierliche Lyman-alpha-Quelle basierend auf Festkörperlasersystemen

In dieser Arbeit wird eine schmalbandige kontinuierliche kohärente Lyman-α-Quelle basierend auf Festkörperlasersystemen zur zukünftigen Kühlung von Antiwasserstoff vorgestellt. Die fundamentalen Festkörperlasersysteme ermöglichen es im Vier-Wellen-Misch-Prozess zur Erzeugung der Lyman-α-Strahlung nicht nur die 6^1S – 7^1S-Zwei-Photonen-Resonanz des Quecksilbers sondern erstmals auch die 6^1S – 6^3P-Ein-Photonen-Resonanz zur Erhöhung der Konversionseffizienz optimal zu nutzen. In ersten Messungen wurden 0,063nW Leistung bei Lyman-α erzeugt. Mit dieser Lyman-α-Quelle war es, durch die Nähe des ersten fundamentalen Lasers zur Ein-Photonen-Resonanz, erstmals möglich den kompletten Verlauf der Phasenanpassungskurve des Vier-Wellen- Misch-Prozesses aufzunehmen. Neben den fundamentalen Lasersystemen und der Lyman-alpha-Erzeugung selbst, wird in dieser Arbeit die Detektion der produzierten Lyman-α-Strahlung mit einem Photomultiplier vorgestellt, die soweit optimiert wurde, dass eine zuverlässige Abschätzung der erzeugten Leistung möglich ist. Für diesen Zweck wurde zudem ein Teststand aufgebaut, mit dem die Transmissivität der Optiken, welche in der Lyman-α-Apparatur verwendet werden, bei 121,56nm gemessen wurde. Des Weiteren wird hier eine vielseitige Rechnung vorgestellt, mit der die erzeugte Leistung bei Lyman-α, unter anderem in Abhängigkeit von der Temperatur, der Absorption des ersten fundamentalen Laserstrahls, dem Dichteprofil des Quecksilberdampfes und unter dem Einfluss eines Puffergases, bestimmt wird.

Computersimulationen zum Einfluss topologischer Beschränkungen auf Polymere

Topologische Beschränkungen beeinflussen die Eigenschaften von Polymeren. Im Rahmen dieser Arbeit wird mit Hilfe von Computersimulationen im Detail untersucht, inwieweit sich die statischen Eigenschaften von kollabierten Polymerringen, Polymerringen in konzentrierten Lösungen und aus Polymerringen aufgebauten Bürsten mit topologischen Beschränkungen von solchen ohne topologische Beschränkungen unterscheiden. Des Weiteren wird analysiert, welchen Einfluss geometrische Beschränkungen auf die topologischen Eigenschaften von einzelnen Polymerketten besitzen. Im ersten Teil der Arbeit geht es um den Einfluss der Topologie auf die Eigenschaften einzelner Polymerketten in verschiedenen Situationen. Da allerdings gerade die effiziente Durchführung von Monte-Carlo-Simulationen von kollabierten Polymerketten eine große Herausforderung darstellt, werden zunächst drei Bridging-Monte-Carlo-Schritte für Gitter- auf Kontinuumsmodelle übertragen. Eine Messung der Effizienz dieser Schritte ergibt einen Beschleunigungsfaktor von bis zu 100 im Vergleich zum herkömmlichen Slithering-Snake-Algorithmus. Darauf folgt die Analyse einer einzelnen, vergröberten Polystyrolkette in sphärischer Geometrie hinsichtlich Verschlaufungen und Knoten. Es wird gezeigt, dass eine signifikante Verknotung der Polystrolkette erst eintritt, wenn der Radius des umgebenden Kapsids kleiner als der Gyrationsradius der Kette ist. Des Weiteren werden sowohl Monte-Carlo- als auch Molekulardynamiksimulationen sehr großer Ringe mit bis zu einer Million Monomeren im kollabierten Zustand durchgeführt. Während die Konfigurationen aus den Monte-Carlo-Simulationen aufgrund der Verwendung der Bridging-Schritte sehr stark verknotet sind, bleiben die Konfigurationen aus den Molekulardynamiksimulationen unverknotet. Hierbei zeigen sich signifikante Unterschiede sowohl in der lokalen als auch in der globalen Struktur der Ringpolymere. Im zweiten Teil der Arbeit wird das Skalierungsverhalten des Gyrationsradius der einzelnen Polymerringe in einer konzentrierten Lösung aus völlig flexiblen Polymerringen im Kontinuum untersucht. Dabei wird der Anfang des asymptotischen Skalierungsverhaltens, welches mit dem Modell des “fractal globules“ konsistent ist, erreicht. Im abschließenden, dritten Teil dieser Arbeit wird das Verhalten von Bürsten aus linearen Polymeren mit dem von Ringpolymerbürsten verglichen. Dabei zeigt sich, dass die Struktur und das Skalierungsverhalten beider Systeme mit identischem Dichteprofil parallel zum Substrat deutlich voneinander abweichen, obwohl die Eigenschaften beider Systeme in Richtung senkrecht zum Substrat übereinstimmen. Der Vergleich des Relaxationsverhaltens einzelner Ketten in herkömmlichen Polymerbürsten und Ringbürsten liefert keine gravierenden Unterschiede. Es stellt sich aber auch heraus, dass die bisher verwendeten Erklärungen zur Relaxationsverhalten von herkömmlichen Bürsten nicht ausreichen, da diese lediglich den anfänglichen Zerfall der Korrelationsfunktion berücksichtigen. Bei der Untersuchung der Dynamik einzelner Monomere in einer herkömmlichen Bürste aus offenen Ketten vom Substrat hin zum offenen Ende zeigt sich, dass die Monomere in der Mitte der Kette die langsamste Relaxation besitzen, obwohl ihre mittlere Verrückung deutlich kleiner als die der freien Endmonomere ist.

Hall-effect thruster-cathode coupling : the effect of cathode position and magnetic field topology

Hall-effect thruster (HET) cathodes are responsible for the generation of the free electrons necessary to initiate and sustain the main plasma discharge and to neutralize the ion beam. The position of the cathode relative to the thruster strongly affects the efficiency of thrust generation. However, the mechanisms by which the position affects the efficiency are not well understood. This dissertation explores the effect of cathode position on HET efficiency. Magnetic field topology is shown to play an important role in the coupling between the cathode plasma and the main discharge plasma. The position of the cathode within the magnetic field affects the ion beam and the plasma properties of the near-field plume, which explains the changes in efficiency of the thruster. Several experiments were conducted which explored the changes of efficiency arising from changes in cathode coupling. In each experiment, the thrust, discharge current, and cathode coupling voltage were monitored while changes in the independent variables of cathode position, cathode mass flow and magnetic field topology were made. From the telemetry data, the efficiency of the HET thrust generation was calculated. Furthermore, several ion beam and plasma properties were measured including ion energy distribution, beam current density profile, near-field plasma potential, electron temperature, and electron density. The ion beam data show how the independent variables affected the quality of ion beam and therefore the efficiency of thrust generation. The measurements of near-field plasma properties partially explain how the changes in ion beam quality arise. The results of the experiments show that cathode position, mass flow, and field topology affect several aspects of the HET operation, especially beam divergence and voltage utilization efficiencies. Furthermore, the experiments show that magnetic field topology is important in the cathode coupling process. In particular, the magnetic field separatrix plays a critical role in impeding the coupling between cathode and HET. Suggested changes to HET thruster designs are provided including ways to improve the position of the separatrix to accommodate the cathode.

A proposed bare tether experiment on board a sounding rocket

A sounding rocket experiment is proposed to carry out two experiments by the conductive bare-tether; 1) the test of the OML (Orbital-Motion-Limited) theory to collect electron, and II) the test of techniques to determine (neutral) density profile in critical E-layer. The main driver of the mission is provide a space tether technology experiment in low-Earth-Orbit (LEO) deploying a long tape tether in space and verify the performance of the bare electrodynamic tape tether. The sounding rocket experiment will show no danger to other satellites as the tether missions YES1, SEDSAT, and ProCEDS, which is cancelled just for afraid of collision with the ISS orbit. Also, the sounding rocket mission is possible to demonstrate the bare tether technology in low cost, simple mission concept, fast realization for space structures. The present sounding rocket experiment is expected to be the first conductive bare tether experiment.

A proposed bare-tether experiment on board a sounding rocket

A mission on board a sounding rocket to carry out two bare-tether experiments is proposed: a test of orbital-motion-limited (OML) collection and the proof-of-flight of a technique to determine the (neutral) density vertical profile in the critical E-layer. Since full bias from the motional field will be small (~ 20V), corresponding to a tape 1 km long and V rocket <8 km/s, a power source with a range of supply voltages of few kV would be used. First, the negative terminal of the supply would be connected to the tape, and the positive terminal to a round, conductive boom of length 10 - 20 m; electrons collected by the boom cross the supply into the tape, where they leak out at the rate of ion impact plus secondary emission. Determination of the density profile from measurements of auroral emissions observed from the rocket, as secondaries racing down the magnetic field reach an E-layer footprint, are discussed. Next the positive terminal of the voltage supply is connected to the tape, and the negative terminal to a Hollow Cathode (HC); electrons now collected by the tape cross the supply, and are ejected at the HC. The opposite connections, with current collection operated by tape and boom, and operating on electrons and ions, and through partial switching in the supply, allow testing OML collection in almost all respects it depends on.

Floating Bare Tether as Upper Atmosphere Probe

Use of a (bare) conductive tape electrically floating in LEO as an effective e-beam source that produces artificial auroras, and is free of problems that have marred standard beams, is considered. Ambient ions impacting the tape with KeV energies over most of its length liberate secondary electrons, which race down the magnetic field and excite neutrals in the E-layer, resulting in auroral emissions. The tether would operate at night-time with both a power supply and a plasma contactor off; power and contactor would be on at daytime for reboost. The optimal tape thickness yielding a minimum mass for an autonomous system is determined; the alternative use of an electric thruster for day reboost, depending on mission duration, is discussed. Measurements of emission brightness from the spacecraft could allow determination of the (neutral) density vertical profile in the critical E-layer; the flux and energy in the beam, varying along the tether, allow imaging line-of-sight integrated emissions that mix effects with altitude-dependent neutral density and lead to a brightness peak in the beam footprint at the E-layer. Difficulties in tomographic inversion, to determine the density profile, result from beam broadening, due to elastic collisions, which flattens the peak, and to the highly nonlinear functional dependency of line-of-sight brightness. Some dynamical issues are discussed.

Structure of the ripple phase in lecithin bilayers.

The phases of the x-ray form factors are derived for the ripple (Pbeta') thermodynamic phase in the lecithin bilayer system. By combining these phases with experimental intensity data, the electron density map of the ripple phase of dimyristoyl-phosphatidylcholine is constructed. The phases are derived by fitting the intensity data to two-dimensional electron density models, which are created by convolving an asymmetric triangular ripple profile with a transbilayer electron density profile. The robustness of the model method is indicated by the result that many different models of the transbilayer profile yield essentially the same phases, except for the weaker, purely ripple (0,k) peaks. Even with this residual ambiguity, the ripple profile is well determined, resulting in 19 angstroms for the ripple amplitude and 10 degrees and 26 degrees for the slopes of the major and the minor sides, respectively. Estimates for the bilayer head-head spacings show that the major side of the ripple is consistent with gel-like structure, and the minor side appears to be thinner with lower electron density.

On the Radial Onset of Clumping in the Wind of the B0I Massive Star QV Nor

We present an analysis of a 78 ks Chandra high-energy transmission gratings observation of the B0I star QV Nor, the massive donor of the wind-accreting pulsar 4U1538−52. The neutron star (NS) orbits its companion in a very close orbit (r < 1.4R*, in units of the stellar radii), thereby allowing probing of the innermost wind regions. The flux of the Fe Kα line during eclipse reduces to only ∼30% of the flux measured out of eclipse. This indicates that the majority of Fe fluorescence must be produced in regions close to the NS, at distances smaller than 1R* from its surface. The fact that the flux of the continuum decreases to only ∼3% during eclipse allows for a high contrast of the Fe Kα line fluorescence during eclipse. The line is not resolved and centered at 1.9368 0.0018 l = 0.0032 - + Å. From the inferred plasma speed limit of v < c l < 800 l D km s−1 and range of ionization parameters of log 1, 2 x = [- ], together with the stellar density profile, we constrain the location of the cold, dense material in the stellar wind of QV Nor using simple geometrical considerations. We then use the Fe Kα line fluorescence as a tracer of wind clumps and determine that these clumps in the stellar wind of QV Nor (B0I) must already be present at radii r < 1.25R*, close to the photosphere of the star.

Galaxy threshing and the origin of ultra-compact dwarf galaxies in the Fornax cluster

A recent all-object spectroscopic survey centred on the Fornax cluster of galaxies has discovered a population of subluminous and extremely compact members, called 'ultra-compact dwarf' (UCD) galaxies. In order to clarify the origin of these objects, we have used self-consistent numerical simulations to study the dynamical evolution a nucleated dwarf galaxy would undergo if orbiting the centre of the Fornax cluster and suffering from its strong tidal gravitational field. We find that the outer stellar components of a nucleated dwarf are removed by the strong tidal field of the cluster, whereas the nucleus manages to survive as a result of its initially compact nature. The developed naked nucleus is found to have physical properties (e. g. size and mass) similar to those observed for UCDs. We also find that although this formation process does not have a strong dependence on the initial total luminosity of the nucleated dwarf, it does depend on the radial density profile of the dark halo in the sense that UCDs are less likely to be formed from dwarfs embedded in dark matter haloes with central 'cuspy' density profiles. Our simulations also suggest that very massive and compact stellar systems can be rapidly and efficiently formed in the central regions of dwarfs through the merging of smaller star clusters. We provide some theoretical predictions on the total number and radial number density profile of UCDs in a cluster and their dependencies on cluster masses.

Non-equilibrium thermodynamics of harmonically trapped bosons

We apply the framework of non-equilibrium quantum thermodynamics to the physics of quenched small-size bosonic quantum gases in a harmonic trap. By studying the temporal behaviour of the Loschmidt echo and of the atomic density profile within the trap, which are informative of the non-equilibrium physics and the correlations among the particles, we establish a link with the statistics of (irreversible) work done on the system. This highlights interesting connections between the degree of inter-particle entanglement and the non-equilibrium thermodynamics of the system.

Análise de DFA e de agrupamento do perfil de densidade de poços de petróleo

In recent years, the DFA introduced by Peng, was established as an important tool capable of detecting long-range autocorrelation in time series with non-stationary. This technique has been successfully applied to various areas such as: Econophysics, Biophysics, Medicine, Physics and Climatology. In this study, we used the DFA technique to obtain the Hurst exponent (H) of the profile of electric density profile (RHOB) of 53 wells resulting from the Field School of Namorados. In this work we want to know if we can or not use H to spatially characterize the spatial data field. Two cases arise: In the first a set of H reflects the local geology, with wells that are geographically closer showing similar H, and then one can use H in geostatistical procedures. In the second case each well has its proper H and the information of the well are uncorrelated, the profiles show only random fluctuations in H that do not show any spatial structure. Cluster analysis is a method widely used in carrying out statistical analysis. In this work we use the non-hierarchy method of k-means. In order to verify whether a set of data generated by the k-means method shows spatial patterns, we create the parameter Ω (index of neighborhood). High Ω shows more aggregated data, low Ω indicates dispersed or data without spatial correlation. With help of this index and the method of Monte Carlo. Using Ω index we verify that random cluster data shows a distribution of Ω that is lower than actual cluster Ω. Thus we conclude that the data of H obtained in 53 wells are grouped and can be used to characterize space patterns. The analysis of curves level confirmed the results of the k-means

An efficient Jeans modelling of axisymmetric galaxies with multiple stellar components

Dynamical models of stellar systems represent a powerful tool to study their internal structure and dynamics, to interpret the observed morphological and kinematical fields, and also to support numerical simulations of their evolution. We present a method especially designed to build axisymmetric Jeans models of galaxies, assumed as stationary and collisionless stellar systems. The aim is the development of a rigorous and flexible modelling procedure of multicomponent galaxies, composed of different stellar and dark matter distributions, and a central supermassive black hole. The stellar components, in particular, are intended to represent different galaxy structures, such as discs, bulges, halos, and can then have different structural (density profile, flattening, mass, scale-length), dynamical (rotation, velocity dispersion anisotropy), and population (age, metallicity, initial mass function, mass-to-light ratio) properties. The theoretical framework supporting the modelling procedure is presented, with the introduction of a suitable nomenclature, and its numerical implementation is discussed, with particular reference to the numerical code JASMINE2, developed for this purpose. We propose an approach for efficiently scaling the contributions in mass, luminosity, and rotational support, of the different matter components, allowing for fast and flexible explorations of the model parameter space. We also offer different methods of the computation of the gravitational potentials associated of the density components, especially convenient for their easier numerical tractability. A few galaxy models are studied, showing internal, and projected, structural and dynamical properties of multicomponent galaxies, with a focus on axisymmetric early-type galaxies with complex kinematical morphologies. The application of galaxy models to the study of initial conditions for hydro-dynamical and $N$-body simulations of galaxy evolution is also addressed, allowing in particular to investigate the large number of interesting combinations of the parameters which determine the structure and dynamics of complex multicomponent stellar systems.

New indicators of star cluster dynamical evolution

This thesis presents a study of globular clusters (GCs), based on analysis of Monte Carlo simulations of globular clusters (GCs) with the aim to define new empirical parameters measurable from observations and able to trace the different phases of their dynamical evolution history. During their long term dynamical evolution, due to mass segregation and and dynamical friction, massive stars transfer kinetic energy to lower-mass objects, causing them to sink toward the cluster center. This continuous transfer of kinetic energy from the core to the outskirts triggers the runaway contraction of the core, known as "core collapse" (CC), followed by episodes of expansion and contraction called gravothermal oscillations. Clearly, such an internal dynamical evolution corresponds to significant variations also of the structure of the system. Determining the dynamical age of a cluster can be challenging as it depends on various internal and external properties. The traditional classification of GCs as CC or post-CC systems relies on detecting a steep power-law cusp in the central density profile, which may not always be reliable due to post-CC oscillations or other processes. In this thesis, based on the normalized cumulative radial distribution (nCRD) within a fraction of the half-mass radius is analyzed, and three diagnostics (A5, P5, and S2.5) are defined. These diagnostics show sensitivity to dynamical evolution and can distinguish pre-CC clusters from post-CC clusters.The analysis performed using multiple simulations with different initial conditions, including varying binary fractions and the presence of dark remnants showed the time variations of the diagnostics follow distinct patterns depending on the binary fraction and the retention or ejection of black holes. This analysis is extended to a larger set of simulations matching the observed properties of Galactic GCs, and the parameters show a potential to distinguish the dynamical stages of the observed clusters as well.