Day 3 :
Keynote Forum
Qiuhe Peng
Nanjing University, China
Keynote: The observed evidence of both invalidating black hole model at the galactic center and magnetic monopole existence
Time : 09:00-09:30
Biography:
Qiuhe Peng is mainly engaged in Nuclear Astrophysics, Particle Astrophysics and Galactic Astronomy research. In the field of Nuclear Astrophysics, his research project involved a neutron star (pulsar), the supernova explosion mechanism and the thermonuclear reaction inside the star, the synthesis of heavy elements and
interstellar radioactive element such as the origin of celestial 26Al. In addition, through his lectures, he establishes Nuclear Astrophysics research in China. He was invited by Peking University, by Tsinghua University (both in Beijing and in Taiwan) and by Nuclear Physics institutes in Beijing, Shanghai, Lanzhou to give lectures on Nuclear Astrophysics for many times. He has participated in the international academic conferences over 40 times and he visited more than 20 countries. In 1994, he visited eight institutes in USA to give lectures. He is the first Chinese Astrophysicist to visit NASA and to give a lecture on the topic, “Nuclear Synthesis of Interstellar 26Al”. In 2005, he visited USA twice and gave lectures in eight universities again. Inviting six Astronomers of USA to give series lectures, he has hosted four consecutive terms summer school on gravitational wave astronomy. After the four-summer school obvious effect, at least 20 young scholars in China in the field of gravitational wave astronomy specialized in learning and research. 220 research papers by him have been published.
Abstract:
According to an abnormally strong radial magnetic field near the GC detected in 2013, we first demonstrate that the radiations observed from the region neighbor of the Galactic Center (GC) is hardly emitted by the gas of accretion disk which is prevented from approaching to the GC by the abnormally strong radial magnetic field. These radiations can't be produced by the black hole at the Center. Secondly, we demonstrate that the abnormally strong radial magnetic field near the GC discovered in 2013 is hardly produced by the α-turbulence dynamo mechanism which is the known most effective dynamo mechanism up to now. The dilemmas of both the black hole model at the GC and the discovery that very strong radial magnetic field in the neighbor of the GC are naturally solved in our model of supermassive object with magnetic monopoles (SMOMM) proposed by Peng and Chou at 2001, in which five predictions had been proposed. Three of these predictions are quantitatively confirmed by later astronomical observations. Thus, we believe that the discovery of abnormally strong radial magnetic field near the GC is probably just the astronomical observational evidence for magnetic monopole existence which is predicted in particle physics. The Conclusions of the paper are: 1) It could be an astronomical observational evidence of the existence of magnetic monopoles which it predicated in particle physics. 2) The black hole model of the GC is invalid. 3) The radiations emitted from the region near the GC may be naturally explained by our model and then our model containing magnetic monopoles could be a reasonable one.
Keynote Forum
Al Zahrani Abdullah
Warsaw University of Technology, Poland
Keynote: Wavy žTheory
Time : 09:30-10:00
Biography:
Al Zahrani Abdullah has completed his Bachelor’s degree in Aero Science from King Fisal Air Academy “KFAA” as a military pilot around 14 years as a pilot in Royal Saudi Air Force. He is the Founder and CEO of Alzahrani Space Innovation, part of Alzahrani International Holding Group SPZOO, Poland. He is interested in Physics, Astrophysics & Space Science and Research in Medicine.
Abstract:
All theories, which describe the beginning of universe, focus on that the universe started with huge explosion, which created everything, while we should ask how galaxies and planets started and black holes were created. We should have a key to understand and proof for that. Which scientists just explain what they want to get in the result, which we already see today? In this paper, I am going to show how I can prove that the universe started with a wave of light, a wave which made the space rubble around and move far away from the source. And during wavy movement galaxies formed and even planets, stars and black holes were formed by curving space only while time is moving smoothly. Through deep looking to the shape and way of movement of the wave we can notice that it is easy to shape galaxies and even black holes. When a galaxy fail to create enough force or gravity to hold together it will just disappear by stronger gravity created by centralized force inside the spherical waves. From that explanation, we can tell that space is moving originally to one direction but the formation of galaxies move in different directions and that is why we see galaxies not rotating around other galaxies. Through this theory, we can tell that galaxies located in certain position share the same properties as other galaxies except properties in time and space like temperature.
- Astronomy | Advanced Software in Astronomy | Space Missions & Satellite
Location: Texas A
Chair
Qiuhe Peng
Nanjing University, China
Co-Chair
Mishra R K
SLIET, India
Session Introduction
Xiaolei Zhang
George Mason University, USA
Title: Collective effects in disk galaxies
Time : 10:00-10:20
Biography:
Xiaolei Zhang obtained her PhD from the University of California, Berkeley, in 1992 and was a Post-doctoral fellow at the Harvard-Smithsonian Center for Astrophysics (CfA) from 1992-1995. She subsequently worked at the CFA as a Staff Scientist, at NASA's Goddard Space Flight Center as a Contractor and at the US Naval Research Lab as a Civil Servant Astrophysicist. She took an early retirement in order to devote more time to her interests in the foundations of physics, in astrophysics, as well as in art. She is currently an Affiliate Faculty at the George Mason University.
Abstract:
Collective effects originate in physical systems going through non-equilibrium phase transitions, which produce selforganised global structures that often serve to accelerate the rates of entropy-increasing thermodynamical evolution of their parent systems. The examples of such emergence behavior and the resulting hierarchical organization of physical laws and phenomena, ranging from models of spontaneous breaking of gauge symmetry in high-energy physics, to the emergence of quasi-particle behavior in condensed matter physics. Emergent behaviors can also be exhibited by classical many-body systems governed by Newtonian laws of gravity. In the case of disk galaxies, we show that the spontaneous emergence of spiral modes is an example of non-equilibrium phase transition, accompanied by the condition of collisionless-shock at the density wave crest. This condition further allows the interaction of matter with the basic state of the galactic disk with the density wave modes, which leads to the stabilization of the modal amplitude growth and the secular radial mass redistribution on the basic state, giving rise to galaxy morphological evolution along the Hubble sequence. It is shown further that well-known classical approaches of applying the Boltzmann kinetic equation, as well as its moment-equation descendants the Euler and Navier-Stokes fluid equations for studying galactic dynamics problems, are inadequate for treating the maintenance of density wave modes as well as the long-term evolution of the morphology of disk galaxies. A global and synthetic approach, incorporating the correlated fluctuations of stars and gas cloud, is adopted to supplement the continuum approach.
Flavia Dell Agli
Instituto de AstrofÃsica de Canarias, Spain
Title: Asymptotic giant branch stars: Dust manufacturers of their host environments
Time : 10:20-10:40
Biography:
Flavia Dell Agli has completed her PhD in Astronomy, at the University of Rome La Sapienza in 2016. She is now a Postdoc at the Instituto de Astrofísica de Canarias. Her main research interest are low-intermediate mass stars and their impact on the history of formation and evolution of different systems. During the last four years she published 22 papers on this topic, six as first author, being involved in several international projects.
Abstract:
During the evolution through the Asymptotic Giant Branch (AGB) phase, low-intermediate mass stars (≤8 Msun) play a fundamental role in the enrichment process of the interstellar medium. The advanced nucleosynthesis active in their internal regions, together with episodes of deep convective mixing, are responsible for a significant variations of the surface chemistry. Furthermore, the low effective temperatures and the high rates of mass loss experienced during the AGB phase favour the formation of cold and dense winds, suitable for the condensation of gas molecules into dust. In this presentation, I will discuss the dust formation process coupled with the description of the AGB evolution and the impact of these stars as dust manufacturers for their host environment.
Xueqing Zhang
Montana Tech of the University of Montana, USA
Title: Study on inversing method of ionospheric properties with spaceborne radar data
Time : 11:00-11:20
Biography:
Xueqing Zhang has completed his PhD from China University of Geology. He is the Assistant Professor of Montana Tech of the University of Montana. He has
published more than 30 papers in the fields of geophysics inversing and radio management.
Abstract:
The fact that ionosphere can effect on radar image and ionospheric effect has become more significant with the increasing interest is noticed. Thus, the geophysical properties of the ionosphere will be embedded in the low-frequency Radar data after the electromagnetic waves transverse through or are reflected by the ionosphere. Correspondingly, the ionospheric major parameters, such as total electron content (TEC), can be inversed from the space-borne radar data. In order to do this, an inversing method for the ionospheric information is put forward. The advantage of data-driven thought is adopted and the strong nonlinear character is considered additionally, while having compared the merits of many different methods, eventually we choose Deep Neural Network (DNN) as the algorithm which can build the relationship between ionosphere and radar data. In machine learning, DNN is a class of deep feed-forward artificial neural networks that has successfully been applied to analyze big data. In this method, the input and output data of DNN are chosen carefully after preprocessing according to the obtainable data and knowledges of experts. The input data are radar data and the output data are the ionospheric parameters. Then training is taken and ended while the error is converged at a certain degree. So far, a model for inversing ionosphere with radar data has been built. At last, the data of radar in a certain area during a certain period of time are input into the trained model and the output data are the interesting information of the ionosphere.
Andreas Eckart
University of Cologne, Germany
Title: The Milky Way’s supermassive black hole: How good a case is it? A challenge for astrophysics and philosophy of science
Biography:
Andreas Eckart is a full Professor for experimental Physics and the Managing Director of the I. Physikalische Institut at the University of Cologne. Since 2006, he is an External Member of the Max-Planck-Institute for Radioastronomy (MPIfR) in Bonn, Germany and Scientific Member of the Max-Planck-Society (MPG). He has also been the Otto Hahn Medal awarded by the Max Planck Society (1984) and the Manne Siegbahn Medal awarded by the Manne Siegbahn Laboratory (2003), Stockholm University, Sweden. Research interests lies in the Galactic Center and nuclei of other galaxies.
Abstract:
The compact and, with 4.3+-0.3 million solar masses, very massive object located at the center of the Milky Way is currently the very best candidate for a supermassive black hole (SMBH) in our immediate vicinity. The strongest evidence for this is provided by measurements of stellar orbits, variable X-ray emission and strongly variable polarized near-infrared emission from the location of the radio source Sagittarius~A* (SgrA*) in the middle of the central stellar cluster. If SgrA* is indeed a SMBH it will, in projection onto the sky, have the largest event horizon and will certainly be the first and most important target of the Event Horizon Telescope (EHT) Very Long Baseline Interferometry (VLBI) observations currently being prepared. These observations in combination with the infrared interferometry experiment GRAVITY at the Very Large Telescope Interferometer (VLTI) and other experiments across the electromagnetic spectrum might yield proof for the presence of a black hole at the center of the Milky Way. It is, however, unclear when the ever mounting evidence for SgrA* being associated with a SMBH will suffice as a convincing proof. Additional compelling evidence may come from future gravitational wave observatories. This manuscript reviews the observational facts, theoretical grounds and conceptual aspects for the case of SgrA* being a black hole. We treat theory and observations in the framework of the philosophical discussions about (Anti) realism and under- determination, as this line of arguments allows us to describe the situation in observational astrophysics with respect to supermassive black holes. Questions concerning the existence of supermassive black holes and in particular SgrA* are discussed using causation as an indispensable element. We show that the results of our investigation are convincingly mapped out by this combination of concepts. Questions concerning the existence of supermassive black holes and in particular SgrA* are discussed using causation as an indispensable element. We show that the results of our investigation are convincingly mapped out by this combination of concepts.
Xiaolei Zhang
George Mason University, USA
Title: Giant impact and the formation of the Colorado Plateau
Time : 11:40-12:00
Biography:
Xiaolei Zhang obtained her PhD from the University of California, Berkeley, in 1992 and was a Post-doctoral fellow at the Harvard-Smithsonian Center for Astrophysics (CfA) from 1992-1995. She subsequently worked at the CFA as a Staff Scientist, at NASA's Goddard Space Flgiht Center as a Contractor and at the US Naval Research Lab as a Civil Servant Astrophysicist. She took an early retirement in order to devote more time to her interests in the foundations of physics, in astrophysics, as well as in art. She is currently an affiliate faculty at the George Mason University.
Abstract:
The Colorado Plateau is an uplifted shallow-bowl shaped high-desert plateau centered on the Four Corners area of the southwestern US, having an area of approximately 130,000 square miles and an elevation ranging from 3000-14000 ft, with an average elevation of 5000 ft. The plateau has the distingushing feature of having been little faulted or folded during the past 600 million years, whereas its immediate outer boundary areas were beset with violent orogenic and igneous activities. We propose and substantiate the hypothesis that the initial formation of the Colorado Plateau was the result of a giant impact event which occurred around 750 million years ago, the consequnce of which included also the split of the Rodinia supercontinent. The impactor was found to be of the size and mass of Planet Mars, which intercepted the Earth'a orbit in an oblique angle, with trajectory roughly in the NE to SW direction with respect to the current orientation of the North America continent. The impactor most likely originated beyond the then-mature Solar System and the impactor's entering of the Solar System's inner confines could be a result of Sun (as well as the stars and interstellar medium in the Solar neighborhood)'s passing through one of the spiral arms or spurs of the Milky Way Galaxy and the resulting perturbative shocks these streaming matters experienced, which further led to the formation of massive stars and their subsequent demise as supernovae, with the blast waves of the supernovae producing (among other things) a rogue extra-Solar planet that invaded the Earth environment. The importance of this process is supported by the observed correlation of the major catastrophic events in Earth's history to the period of the Solar system's orbit in the Milky Way Galaxy and thus to the period of the Solar' System's crossing of the Galactic spiral arms. The Earth's tectonic history thus appears to be intimately linked to the Solar System's motion within the Galactic environment.
Jakub Nikonowicz
Poznań University of Technology, Poland
Title: Stable field detection as a novel method for blind sensing of weak radio signals
Time : 12:00-12:20
Biography:
Jakub Nikonowicz has received his MSc degree in electronics and telecommunication engineering from the Poznań University of Technology in 2014. Since September 2014, he is a PhD student at the Faculty of Electronics and Telecommunications. His current research interest lies in the field of signal processing for spectrum sensing and blind signal detection.
Abstract:
Since the discovery of space radio waves in the early 1930s, most astronomical objects have been perceived as radio waves sources. Radio-astronomy observations ultimately consist in measuring the energy received from a distant source, with particular emphasis on the detection of unknown and weak signals. The most commonly used blind detection method relies on energy detection with noise power estimation. The variability of the radio environment, however, greatly complicates the entire detection process. In order to solve the problem of detection in varying noise conditions, we propose a novel method of blind signal detection called Stable Field Detection (SFD), which does not require any knowledge of the noise variance. The proposed method uses the bin value distribution of the received signal’s power spectrum density and the moving average. It refers to the mutual relations between the distributions of random variables to extract more information from the spectrum than normal energy detection. As a result, SFD operates on thresholding Gaussian distribution, which makes it as easy to use as energy detection, but remains much more effective. The simulation results for radio pulses show that the performance of the method is significantly improved under the proposed scheme. With regard to weak signals, when compared to the energy detection, the lower limit of the permissible signal-to-noise ratio has been decreased by 4dB. At the same time, the proposed solution maintains low O (nlogn) computational complexity. SFD is considered a new, effective and simple software defined detector that addresses the challenges of modern astronomy.
Qiuhe Peng
Nanjing University, China
Title: Implication of strong magnetic field near the galactic center (GC)
Time : 12:20-12:40
Biography:
Qiuhe Peng is mainly engaged in Nuclear Astrophysics, Particle Astrophysics and Galactic Astronomy research. In the field of Nuclear Astrophysics, his research project involved a neutron star (pulsar), the supernova explosion mechanism and the thermonuclear reaction inside the star, the synthesis of heavy elements and interstellar radioactive element such as the origin of celestial 26Al. In addition, through his lectures, he establishes Nuclear Astrophysics research in China. He was invited by Peking University, by Tsinghua University (both in Beijing and in Taiwan) and by Nuclear Physics institutes in Beijing, Shanghai, Lanzhou to give lectures on Nuclear Astrophysics for many times. He has participated in the international academic conferences over 40 times and he has visited more than 20 countries. In
1994, he visited eight institutes in USA to give lectures. He is the first Chinese Astrophysicist to visit NASA and to give a lecture on the topic, Nuclear Synthesis of Interstellar 26Al. In 2005, he visited USA twice and gave lectures in eight universities again. Inviting six astronomers of USA to give series lectures, he has hosted four consecutive terms summer school on gravitational wave astronomy. After the four-summer school obvious effect, at least 20 young scholars in China in the field of gravitational wave astronomy specialized learning and research. He has published 220 research papers.
Abstract:
A key observation has been reported in 2013; an abnormally strong radial magnetic field near the GC is discovered. Firstly, we demonstrate that the radiations observed from the GC are hardly emitted by the gas of accretion disk which is prevented from approaching to the GC by the abnormally strong radial magnetic field and these radiations can't be emitted by the black hole model at the Center. However, the dilemma of the black hole model at the GC is naturally solved in our model of super massive object with magnetic monopoles (MMs). Three predictions in our model are quantitatively in agreement with observations: 1.) Plenty of positrons are produced from the direction of the GC with the rate is 6 × 1042 e+/sec or so. This prediction is quantitatively confirmed by observation {(3.4-6.30) ×1042 e+ sec-1}. 2.) A strong radial magnetic field is generated by some magnetic monopoles condensed in the core region of the super massive object. The magnetic field strength at the surface of the object is about 20-100 Gauss at 1.1×104 Rs (Rs is the Schwarzschild radius) or B ≈ (10-50) mG at r = 0.12pc. This prediction is quantitatively in agreement with the lower limit of the observed magnetic field ≥8mG. 3.) The surface temperature of the super-massive object in the Galactic center is about 120 K and the corresponding spectrum peak of the thermal radiation is at 1013 Hz in the sub-mm wavelength regime. This is quantitatively basically consistent with the recent observation. The conclusions are that it could be an astronomical observational evidence of the existence of MMs and no black hole is at the GC. Besides, making use of both the estimations for the space flux of MMs and nucleon decay catalyzed by MMs (called the RC effect) to obtain the luminosity of celestial objects by the RC effect. In terms of the formula for this RC luminosity we are able to present a unified treatment for various kinds of core collapsed supernovae, SNII, SNIb, SNIc, SLSN and the production mechanism for γ ray burst, as well as the heat source of the Earth’s core, the energy source needed for the white dwarf interior. This unified model can also be used to reasonably explain the possible association of the shot γ ray burst detected by the Fermi γ ray Burst Monitoring Satellite (GBM) with the September 2015 LIGO gravitational wave event GW150914.
Mishra R K
SLIET, India
Title: Comparative studies of cosmological models in alternative theory of gravity with LVDP and BVDP
Time : 12:40-13:00
Biography:
Mishra R K has completed his PhD from DDU Gorakhpur University and joined as Lecturer at Department of Mathematics, SLIET Deemed University, Longowal, District Sangrur and Punjab in January 2000. At present, he is working as Professor, Department of Mathematics, SLIET Deemed University, Longowal, Punjab, India. One of the premier institutes established and funded by Government of India. He has published more than 50 Research papers in reputed journals and has been serving as an Editorial Board Member of repute. Apart from his teaching and active participation in Research (In area of Cosmology) he is also helping the institute in various administrative responsibilities. At present, he is also working as Head, Department of Training and Placement SLIET.
Abstract:
The study of cosmological models with time dependent deceleration parameter attracts researchers after the discovery of accelerating expansion of universe confirmed by two independent teams. The variable deceleration parameter has much importance to measure the expansion rate. Therefore, the investigation of various cosmological models with time dependent deceleration parameter indicates new sector in theoretical cosmology. From literature it is also noticed that Berman (1998) has been studied the cosmological models with constant DP and proposed a law for constant deceleration parameter (CDP) as q = m−1, here m is arbitrary constant. After this work several researchers derived and investigated cosmological models by assuming the time-varying DP. In this communication we have presented a comparative study of Friedmann-Lemaˆitre-Robertson -Walker (FLRW) cosmological models in alternative theory of gravity with linearly varying deceleration parameter (LVDP) and bi-linearly varying deceleration parameter (BVDP) as suggested by Mishra et al. The role of viscosity in cosmology have been studied by several researchers in past. Under the influence of such study we have also studied bulk viscous fluid cosmological models in alternative f (R, T) theory of gravity along with comparison of results by taking LVDP and BVDP. The main conclusion of the paper is that BVDP law provides better results in comparative with Berman's constant deceleration law (CDP) and LVDP law.
Eiji Akiyama
National Astronomical Observatory of Japan, Japan
Title: Observational signature of grain growth in the protoplanetary disk around young star LkHα 330
Time : 14:00-14:20
Biography:
Eiji Akiyama has obtained his PhD in 2012 from Ibaraki University, Japan. He has been working as a Science Staff of the Atacama Large Millimeter/submillimeter Array (ALMA) international project. He has published around 40 papers covering planet formation and exoplanets based on observations of near infrared and millimeter/submillimeter wavelength. He recently won the Outstanding Young Scientist award 2016 from the Japanese Society of Planetary Science.
Abstract:
Grain growth is an initial step toward planet formation since it involves the coagulation of approximately micron-sized dust, resulting in planetesimals and finally planets. We have conducted H-band (1.6 μm) linear polarimetric observations by Subaru telescope and 0.88 mm interferometric observations by Submillimeter Array toward a transitional disk around the intermediate-mass pre-main sequence star LkHα 330. The observations show a pair of asymmetric spiral arms in the disk, suggesting that a massive unseen (proto)planet exists in the disk as indicated by recent global hydro simulations. The possibility of grain growth that can generate the asymmetric structure was investigated through the opacity index (β) from the observed slope of the spectral energy distribution between 0.88 mm and 1.3 mm wavelength taken by several interferometric observations. The results imply that grains are indistinguishable from the interstellar medium dust in the east side (β~2.0), but much smaller in the west side (β~0.7), indicating differential grain growth or dust trapping in the spiral arms. Combining the results of near-infrared and submillimeter observations, we find that the spiral arm is geometrically thick and grains grow to millimeter size near the disk mid-plane. Future observations at centimeter wavelength and differential polarization imaging in other bands (Y to K) with extreme adaptive optics imagers are required to understand how large dust grains form and to further explore the dust distribution in the disk.
Yu-Qing Lou
Tsinghua University, China
Title: Hypermassive black holes in the universe
Time : 14:20-14:40
Biography:
Yu-Qing Lou is the winner of 1981 China-US Physics Examination and Application (CUSPEA) sponsored by T D Lee. He has completed his Physics PhD in 1987 from Havard University. He became High Altitude Observatory and Advanced Study Program Fellow at National Center for Atmospheric Research (NCAR) 1987-1989. He has published in more than 140 international journal papers (including Nature, Science, The Astrophysical Journal (Letters), Monthly Notices of the Royal Astronomical Society (Letters), Journal of Geophysical Research, Geophysical Research Letters, Astronomy and Astrophysics). In 2002, he became distinguished Yangtze Professor in Physics Department of Tsinghua University. He has served in Review Panels in USA, China and others.
Abstract:
In reference to supermassive black holes (SMBHs) in the mass range of millions to several billions of solar masses, we predicted hypermassive black holes (HMBHs) in the mass range of 10 to 1000 billions of solar masses and possibly even higher in the universe including the early universe as results of dynamic gravitational collapses of sufficiently large mass reservoirs. Observational evidence, consequences and implications of HMBHs and SMBHs in the universe are presented. We indicate generation of gravitational waves by inevitable convective and circulative turbulence, magneto-hydrodynamic (MHD) dynamo processes, acceleration of ultra-high energy cosmic rays (UHECRs), bursts of electromagnetic waves when random magnetic fields are involved in such dynamic gravitational collapses. We discuss dark matter black holes (DMBHs) and mixed matter black holes (MMBHs) in the Universe including the early Universe. We also show the possibility of forming chains of gravitationally collapsed on various mass scales. It is anticipated that Hubble Space Telescope, James Webb Space Telescope, LOFAR, Square Kilometer Array and so forth can provide more valuable diagnostic clues of HMBHs and SMBHs.
Bipin Singh Koranga
University of Delhi, India
Title: Neutrino mixing in matter at extremely high energies
Time : 14:40-15:00
Biography:
Bipin Singh Koranga is currently working in as Assistant Professor in Department of Physics, Kirori Mal College, University of Delhi, USA. He has extended his valuable service in field of Nuclear Physics, Neutrino Physics and Cosmology for several years and has been a recipient of many award and grants. His international experience includes various programs, contributions and participation in different countries for diverse fields of study. His research interests reflect in his wide range of publications in various national and international journals.
Abstract:
We have studied neutrino mixing at extreme high energy considering two flavor frameworks with matter effects. We analyze the atmospheric neutrino data within the simplest scheme of two neutrino oscillation. We consider as special case of matter density profile, which are relevant for neutrino oscillations. In particular, we compute to constrain a specific form of neutrino mass square difference and mixing in extreme high energy in matter. The dispersion relations for the neutrino mixing in neutrino oscillation in matter are discussed.
- Video Presentations
Location: Texas A
Session Introduction
Wei Peng-Sheng
National Sun Yat-Sen University, Taiwan
Title: Absorption coefficient across atmospheric troposphere layer
Time : 15:00-15:15
Biography:
Wei Peng-Sheng has received his PhD in Mechanical Engineering Department at University of California, Davis. He has been a Professor in the Department of Mechanical and Electro-Mechanical Engineering of National Sun Yat-Sen University, Kaohsiung, Taiwan, since 1989. He has contributed to advancing the understanding of and to the applications of electron and laser beam, plasma and resistance welding through theoretical analyses coupled with verification experiments and investigations also include studies of their thermal and fluid flow processes and formations of the defects such as humping, rippling, spiking and porosity. He has published more than 80 SCI journal papers, given keynote or invited speeches in international conferences more than 110 times. He is a Fellow of AWS (2007) and a Fellow of ASME (2000). He also received the Outstanding Research Achievement Awards from both the National Science Council (2004) and NSYSU (1991, 2001, 2004), the Outstanding Scholar Research Project Winner Award from National Science Council (2008), the Adams Memorial Membership Award from AWS (2008), the Warren F Savage Memorial Award from AWS (2012) and the William Irrgang Memorial Award from AWS (2014). He has been the Xi-Wan Chair Professor of NSYSU since 2009 and Invited Distinguished Professor in the Beijing University of Technology, China, during 2015-2017.
Abstract:
The absorption coefficient of carbon dioxide is responsible for temperature in the troposphere layer, which is less than the altitude of 10 km in the atmosphere, is presented in this work. It has been well known that the solar irradiation can penetrate through the troposphere layer within short wavelength range near the visible range. It can be absorbed, scattered by the atmosphere and absorbed and reflected by the earth ground. The ground emits radiation in the ranges of long wavelengths. In the presence of carbon dioxide and other emission gases, the atmosphere layer acting as the glass of a greenhouse increases temperature of the atmosphere. Even though global warming strongly affects the life of the human being, the cause of global warming is still controversial. This work thus establishes a fundamental, systematical and quantitative analysis of absorption coefficient of carbon dioxide across the troposphere layer. Absorption coefficient is a function of wavelength, temperature and concentration. Carbon dioxide is absorbed in long wavelength bands centered at 15, 10.4, 9.4, 4.3, 2.7 and 2.0 micrometers, respectively. The predict absorption coefficients agree with experimental and theoretical results in the exponential wide band model in different bands. The computed results are confirmed by experimental data, revealing the effects of carbon dioxide on temperatures in the troposphere.
Hans Joerg Fahr
University of Bonn, Germany
Title: The fate and role of freely propagating cosmic photons in expanding universes
Time : 15:15-15:30
Biography:
Hans Joerg Fahr is Full Professor for Astrophysics at the University of Bonn in Germany, was President of Comm.21 of the IAU and received the National First Class award of Germany in 2003. At present he is Co-I of the NASA Satellites TWINS and IBEX.
Abstract:
According to present cosmological views the energy density of CMB (Cosmic Microwave Background ) photons , freely propagating through the expanding universe, varies inversely proportional to the fourth power of the cosmic scale S . This is expected because GRT in application to FLRW (Friedman-Lemaitre-Robertson-Walker)- universes seems to be able to show that photons undergo a
cosmological redshift which together with the decrease of photon densities leads to the expected S^(-4) behavior. This conclusion appears to reasonably well explain the presently observed Planckian CMB spectrum with its actual temperature of T(CMB)=2.7 K , while at the time of the CMB origin, when cosmic matter recombined, its temperature would have been about 3000 K when the scale of the universe was smaller by a factor of (1/1100). In this talk we shall question whether the scale-dependence of the CMB energy density entering the energy-momentum tensor falls off like S^(-4). For that purpoe we investigate on a new physical basis whether the wavelengths of freely propagating cosmic photons during their travels up to the present day have permanently been redshifted or their redshift only becomes apparent when CMB photons are registered by spectrometers (clocks) at these present days. We do show that photons in its own reference system cannot change their proper state, but keep their proper energy while freely propagating. This
implies that the photon energy density only decreases as S^(-3) , as does the baryonic matter density. This, however, then means that both baryon and photon energy densities, entering the energy momentum tensor, do behave absolutely alike what concerns their dependence on S and hence in solutions for the cosmic expansion dynamics ,even at present days, CMB photons cannot be neglected. We nevertheless also show that such cosmic photons when registered at these days are judged as redshifted photons explaining why the presentday CMB is a Planckian radiation with the temperature of only 2.7 K.
V G Plekhanov
Fonoriton Sci Lab, Estonia
Title: Direct observation of the strong (nuclear) interaction in the optical spectra of solids
Time : 15:30-15:45
Biography:
V G Plekhanov is graduated from Tartu State University in 1968, PhD (Physics and Mathematics) and Doctor of Science (Physics and Mathematics). His main interest fields: the origin of the mass (quantization of matter) as well as the experimental manifestation of the strong nuclear interaction in the spectroscopy of solids. He is author 197 publications both in English and Russian. His main books involve: Isotope effects in solid state Physics (Academic Press, San Diego, 2001). Isotope - Based Quantum Inormation (Springer, Heidelberg, 2012). Isotope Effects: Physics and Applications (Palmarium Academic Press, Saarbrucken, Deutschland, 2014) (in Russian), Isotopes in Condensed Matter (Springer, Heidelberg, 2013) and Isotope effect- Macroscopical manifestation of the strong interaction (Lambert Academic Publishing, Deutschland, 2017) (in Russian).
Abstract:
Up to the present time, the macroscopical manifestation of the strong (nuclear) interaction is limited by radioactivity and the release of nuclear energy. Our communication is devoted to the description of the new mechanism to the strong force manifestation. Activation of the strong interaction by adding of one neutron to the nucleus causes the global reconstruction of the macroscopic characteristics of solids. We have studied the low-temperature optical spectra of the LiH and LiD crystals which differ by the term of one neutron from each other. As demonstrated early, most low-energy electron excitation in LiH crystals are largeradius excitons. Because of the high reactivity and high hygroscopy of investigated crystals, an efficient protection against atmosphere was necessity. Taking into account this circumstance we have developed special equipment which is allowed to prepare samples with clean surface cleaving in the bath of helium cryostat with normal or superfluid liquid helium. The samples with such surface allow performing measurements for 15 hours. Exciton luminescence is observed when LiH crystals are excited in the midst of fundamental absorption. The spectrum of exciton photoluminescence of LiH crystals cleaved in superfluid helium consists of narrow phonon-less emission line and its broader phonon replicas which arise due to radiative annihilation of excitons with the production of one to five LO phonons. As an example, the picture shows the low-temperature (T=2K) photoluminescence spectra of LiH and LiD crystals. Comparison the experimental results on the luminescence spectra in the crystals which differ by a neutron only is allowed to the next conclusions. At the adding one neutron (using LiD crystals instead LiH ones) is involved the increase exciton energy on 103 meV. At the addition one neutron the energy of LO phonons are decreased on the 36 meV that is direct seen also from luminescence spectra. As far as the gravitation, electromagnetic and weak interactions are the same of both crystals it only changes the strong interaction
therefore a logical conclusion is made that the renormalization of the energy of electromagnetic excitations (excitons, phonons) is carried out by the strong (nuclear) interaction. The last conclusion opens new avenue in the investigations of the strong (nuclear) interaction using by means the condensed matter alike traditional nuclear methods (including accelerating technique).
Hafiza Rizwana Kausar
University of Central Punjab, Pakistan
Title: Transportation process in the gravitational collapse
Time : 15:45-16:00
Biography:
Hafiza Rizwana Kausar has completed her PhD in 2012 in Einstein’s Theory of Relativity from University of the Punjab, Pakistan and postdoctoral studies from Department of Physics, University of Zurich, Switzerland. Her research articles have been published in regular journals of international repute having 50 plus impavt factor. She got research awards by Pakistan Council for Science and Technology in 2012 and 2015 of category F and B respectively. She has presented her work at various national and international conferences. Currently, she is working at the University of Central Punjab (UCP) Lahore as the Incharge Faculty of Sciences and Director of Centre for Applicable Mathematics and Statistics in the UCP Business School.
Abstract:
In this paper, we study the transport equation which provide the information about the transfer of mass, heat and momentum during the gravitational collapse of massive stars. We adopt the modified theories of gravity and examine the process of energy transport and its effects on the collapsing process. We discuss how such theories may incorporated mathematically into the analysisand control of the dynamics of a complex system. The transport equation governs the dissipative fluxes and their associated quantities like temperature, relaxation time and thermal conductivity. It helps to construct physically viable models of radiating stars. We also develop the dynamical equations and coupled with transport equation. We discuss how inertia of heat causes a decrease in the inertial and gravitational mass densities and hence effect the outcome of the gravitational collapse. We obtained three cases depending on a physical factor and on its positive and negative value. Positive value yields the gravitational collapse of massive stars whereas negative value yields the formation of white dwarf.