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Journal articles on the topic 'Star heat'

Author: Grafiati

Published: 6 September 2023

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1

Andersson, Nils. "Neutron star seismology." Proceedings of the International Astronomical Union 8, S291 (August 2012): 159. http://dx.doi.org/10.1017/s1743921312023472.

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AbstractI will provide an overview of recent improvements in our models for vibrating neutron stars, discussing the role of composition, heat, crust elasticity and superfluidity. I will explain how the results may impact on observations, in particular related to magnetar QPOs and future gravitational-wave searches.

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2

Noor H. Dhaher, Mohammed K. Khashan, and Nawfel Muhammed Baqer Muhsin. "One Dimensional Steady-State Heat Transfer on a Star Fin Shape." CFD Letters 14, no. 12 (November 18, 2022): 1–10. http://dx.doi.org/10.37934/cfdl.14.12.110.

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The convection heat transfers on a surface exposed to the fluid may be enhanced by attaching to the surface, known as the fins. To keep the system stable, heat transmission via solids, boundaries, or walls must be continuously dissipated to the environment or surroundings. A large quantity of heat must be dissipated from a small space in many engineering applications. A fin can boost the surface area’s effectiveness; hence, maximize convectional heat. Two shapes of straight aluminum fins have been used, cylindrical and star shape. The result shows that the star fins are appealing due to the same diameter and length; it has a lot more heat transfer than a cylindrical fin. In electronic devices, cylindrical and star fins are provided on the surface of the processor device. The result is done by SolidWorks simulation with 300 ºC on the surface as well as cylindrical and star fin. Input parameters like thermal conductivity, heat transfer coefficient, as well as fin’s density and dimensions are measured. The temperature distribution, heat flow, as well as heat flux all resembles output parameters.

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3

Bošnjaković, Mladen, Ante Čikić, Simon Muhič, and Mario Holik. "Heat Transfer Correlations for Star-Shaped Fins." Applied Sciences 11, no. 13 (June 25, 2021): 5912. http://dx.doi.org/10.3390/app11135912.

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Star-shaped fins are a newer type of fin for which correlations for heat transfer and pressure drop do not yet exist in the literature. Therefore, correlation equations for air-side heat transfer and pressure drop in a finned heat exchanger with star-shaped stainless-steel fins in staggered arrangement were developed in this work. To obtain these correlations, a numerical analysis of the basic heat exchanger geometry and another 21 variants of heat exchanger geometry was performed using computational fluid dynamics, and then the results of laboratory tests of a model of heat exchangers with star-shaped fins were used. In the numerical analysis, the fin pitch, the fin thickness, and the air velocity at the inlet to the heat exchanger were varied. The Nusselt (Nu) and Euler (Eu) numbers were determined for each variation analyzed. Initial correlations for Nu and Eu were derived using the least-squares deviation method. The correlation coefficients thus obtained were adjusted to agree with the results of the laboratory tests. The deviation of the final obtained correlation for Nu from the experimental test results was up to 10% in the range of Re < 3500, whereas for higher values of Re, the deviation was less than 2%. The Eu correlation deviated from experimental results up to 19% in the range of Re < 4000, whereas in the range of Re > 5600, the deviation was less than 1%. The correlations were valid in the range 2000 < Re < 16,000.

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4

Lazzari, G., and F. V. De Blasio. "Heat diffusion time in neutron star crusts." Astrophysics and Space Science 229, no. 2 (July 1995): 311–16. http://dx.doi.org/10.1007/bf00626872.

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5

Hui, C. Y., and K. S. Cheng. "Anisotropic Heat Transfer Inside Rotating Neutron Stars." Symposium - International Astronomical Union 218 (2004): 39–40. http://dx.doi.org/10.1017/s0074180900180520.

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We have developed the anisotropic heat transport equation for rotating neutron stars. With a simple model of neutron star, we also model the propagation of heat pulses resulting from transient energy releases inside the star. Even in the slow rotation limit, the results with rotational effects involved could differ significantly from those obtained with a spherically symmetric metric in the timescale of the thermal afterglow.

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6

GOVENDER, M., K. S. GOVINDER, S. D. MAHARAJ, R. SHARMA, S. MUKHERJEE, and T. K. DEY. "RADIATING SPHERICAL COLLAPSE WITH HEAT FLOW." International Journal of Modern Physics D 12, no. 04 (April 2003): 667–76. http://dx.doi.org/10.1142/s0218271803003086.

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We present here a simple model of radiative gravitational collapse with radial heat flux which describes qualitatively the stages close to the formation of a superdense cold star. Starting with a static general solution for a cold star, the model can generate solutions for the earlier evolutionary stages. The temporal evolution of the model is specified by solving the junction conditions appropriate for radiating gravitational collapse. The results will be useful in constructing models for the evolution of X-ray pulsars, like Her X-1.

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7

Yost, D. A., R. K. Burkhard, and R. C. Hoseney. "Heat-Burst Calorimetry of Heated Starch." Starch - Stärke 38, no. 11 (1986): 366–68. http://dx.doi.org/10.1002/star.19860381102.

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8

Dorokhov, A. S., А. G. Aksenov, A. V. Sibirev, M. A. Mosyakov, and N. V. Sazonov. "Study of an Exhaust Gas Heat Separation System for the Beet Harvester." Agricultural Machinery and Technologies 16, no. 1 (March 18, 2022): 19–26. http://dx.doi.org/10.22314/2073-7599-2022-16-1-19-26.

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It was noted that increased soil moisture worsens the quality of harvesting root crops due to a decrease in the completeness of separation. To increase the separating capacity of a slotted cleaner for root crops, it was proposed to improve the heating of the separating surface with hot exhaust gas. (Research purpose) To optimize the design and technological parameters of an exhaust gas heat separation system of the sugar beet harvester power plant. (Materials and methods) Federal Scientific Agroengineering Center VIM developed an exhaust gas heat separation system for harvesting root crops and potatoes in high moisture conditions using the heat of the harvester power plant exhaust gases. The cleaning quality of the separating system of a self-propelled sugar beet harvester was determined under the gradual engine load from 0 to 100 percent of the nominal rated power. The temperature of the exhaust gases was measured with the assumption of changes in the engine load and its effective power. (Results and discussion) The experiment revealed an increase in the completeness of the separation of a root crops heap from 96.0 to 98.8 percent at 26-32 percent soil moisture due to the separation system in the form of a cleaning star, which uses the heat of the engine exhaust gases. The established optimal values of the factors under consideration are as follows: the separating star rotation rate is 21.8 revolutions per minute, the distance between the separating star and the deflector is 128.4 millimeters. (Conclusions) It was determined that the high quality of the technological process of root crops harvesting in high soil moisture conditions ensuring a 97-percent separation efficiency is possible if optimize the separating device design and technological parameters and maintain the separating star rotation rate at 20-22 revolutions per minute and the distance between the separating star and the deflector within 120-140 millimeters. The authors noted the prospects of developing this system and the need for theoretical and experimental studies to improve the design and technological process of the harvester separating system.

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9

Urpin, V. "Neutron star oceans: Instability, mixing, and heat transport." Astronomy & Astrophysics 421, no. 1 (June 11, 2004): L5—L8. http://dx.doi.org/10.1051/0004-6361:20040165.

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10

Bošnjaković, M., A. Čikić, S. Muhič, and M. Stojkov. "Tube heat exchanger with new star shaped fins." IOP Conference Series: Materials Science and Engineering 393 (August 10, 2018): 012071. http://dx.doi.org/10.1088/1757-899x/393/1/012071.

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11

Jiranuntakul, Wittawat, Chureerat Puttanlek, Vilai Rungsardthong, Santhanee Puncha-arnon, and Dudsadee Uttapap. "Amylopectin structure of heat-moisture treated starches." Starch - Stärke 64, no. 6 (February 29, 2012): 470–80. http://dx.doi.org/10.1002/star.201100160.

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12

Talwar, S. P., and M. P. Bora. "Thermal instability in a star—gas system." Journal of Plasma Physics 54, no. 2 (October 1995): 157–72. http://dx.doi.org/10.1017/s0022377800018420.

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A composite interstellar model consisting of stars and optically thin radiating plasma is considered in order to investigate the thermal instability arising from possible radiation and other heat-loss mechanisms. The stellar dynamics is governed by the Vlasov equation, while the gas is supposed to be a hydromagnetic plasma, described by the MHD equations, with a density- and temperature-dependent heat-loss function. It is shown that while with cold stars the system is in general unstable irrespective of thermal effects of the plasma, with warm stars having a Maxwellian distribution the thermal plasma considerably influences the stability of the composite system. It is also shown that the otherwise stable composite (with warm stars) configuration may become unstable in the presence of a radiating plasma because of coupling between the heat-loss mechanisms and stellar populations.

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13

NAIDU, N. F., M. GOVENDER, and K. S. GOVINDER. "THERMAL EVOLUTION OF A RADIATING ANISOTROPIC STAR WITH SHEAR." International Journal of Modern Physics D 15, no. 07 (July 2006): 1053–65. http://dx.doi.org/10.1142/s0218271806008760.

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We study the effects of pressure anisotropy and heat dissipation in a spherically symmetric radiating star undergoing gravitational collapse. An exact solution of the Einstein field equations is presented in which the model has a Friedmann-like limit when the heat flux vanishes. The behavior of the temperature profile of the evolving star is investigated within the framework of causal thermodynamics. In particular, we show that there are significant differences between the relaxation time for the heat flux and the relaxation time for the shear stress.

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14

Naylor, T., and M. W. Somers. "The Effect of the Nova Explosion on the Evolution of Cataclysmic Variables." International Astronomical Union Colloquium 163 (1997): 771–72. http://dx.doi.org/10.1017/s0252921100043906.

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Classical nova outbursts are thermonuclear explosions on the surfaces of the white dwarfs in cataclysmic variables. The explosion heats the surface layers of the white dwarf, which are expected to cool on a timescale of a hundred years. The hot white dwarf should have two obvious effects on the system.(1)It will heat the surface of the accretion disc and secondary star, increasing the overall luminosity of the system.(2)By irradiating the surface of the secondary star it may bloat it and drive more mass transfer, thus again increasing the overall luminosity.

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15

Bošnjaković, Mladen, and Simon Muhič. "Numerical Analysis of Tube Heat Exchanger with Trimmed Star-Shaped Fins." Applied Sciences 12, no. 10 (May 11, 2022): 4857. http://dx.doi.org/10.3390/app12104857.

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In some engineering applications, it is very desirable that the heat exchanger is as light as possible while maintaining the heat transfer rate at an acceptable level. In this context, the possibility of reducing the weight of the heat exchanger with the star-shaped fins by cutting off the thermally least efficient part of the fin was investigated. For this purpose, the rear part of the fins was trimmed to Ø28, Ø31 and Ø34 mm. Numerical analysis was used to determine the influence of each variant on the flow characteristics in the air–water heat exchanger and on heat transfer for the range of 2300 < Re < 16,000. The best results were obtained by trimming the rear part of the fin to Ø28 mm. With a 5.53% reduction in fin weight, heat transfer can be increased by up to 8.12% compared to the star-shaped fins without trimming. The pressure drop can be reduced by up to 0.92%. The trimmed fins were also compared with perforated star-shaped fins (perforation Ø2). At approximately the same weight, the trimmed fins increase the heat transfer coefficient by up to 5.75% with a reduction in pressure drop of up to 0.76% compared to the perforated fins.

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16

Liu, X. W., J. D. Liang, R. X. Xu, J. L. Han, and G. J. Qiao. "The missing compact star of SN1987A: a solid quark star?" Proceedings of the International Astronomical Union 8, S291 (August 2012): 448–50. http://dx.doi.org/10.1017/s1743921312024465.

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AbstractTo investigate the missing compact star of Supernova 1987A, we analyzed the cooling and heating processes of a possible compact star based on the upper limit of observational X-ray luminosity. From the cooling process, we found that a solid quark-cluster star (SQS), having a stiffer equation of state than that of a conventional liquid quark star, has a heat capacity much smaller than a neutron star. The SQS can cool down quickly, naturally explaining the non-detection of a point source in X-ray wavelengths. On the other hand, we considered the heating processes due to magnetospheric activity and possible accretion and obtained some constraints on the parameters of a possible pulsar. Therefore, we concluded that a SQS can explain the observational limit in a confident parameter space. As a possible central compact object, the pulsar parameter constraints can be tested for SN1987A with advanced, future facilities.

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17

Bošnjaković, Mladen, and Simon Muhič. "Numerical Analysis of Tube Heat Exchanger with Perforated Star-Shaped Fins." Fluids 5, no. 4 (December 13, 2020): 242. http://dx.doi.org/10.3390/fluids5040242.

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This article discusses the possibility of further reducing the mass of the heat exchanger with stainless steel star-shaped fins while achieving good heat transfer performance. For this purpose, we perforated the fins with holes Ø2, Ø3, and Ø4 mm. Applying computational fluid dynamics (CFD) numerical analysis, we determined the influence of each perforation on the characteristics of the flow field in the liquid–gas type of heat exchanger and the heat transfer for the range of Re numbers from 2300 to 16,000. With a reduction in the mass of the fins to 17.65% (by Ø4 mm), perforated fins had greater heat transfer from 5.5% to 11.3% than fins without perforation. A comparison of perforated star-shaped fins with annular fins was also performed. Perforated fins had 51.8% less mass than annular fins, with an increase in heat transfer up to 26.5% in terms of Nusselt number.

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18

GOVENDER, M. "NONADIABATIC SPHERICAL COLLAPSE WITH A TWO-FLUID ATMOSPHERE." International Journal of Modern Physics D 22, no. 07 (June 2013): 1350049. http://dx.doi.org/10.1142/s0218271813500491.

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In this paper, we present an exact model of a spherically symmetric star undergoing dissipative collapse in the form of a radial heat flux. The interior of the star is matched smoothly to the generalized Vaidya line element representing a two-fluid atmosphere comprising null radiation and a string fluid. The influence of the string density on the thermal behavior of the model is investigated by employing a causal heat transport equation of Maxwell–Cattaneo form.

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19

Mu, Tai-Hua, Oluwaseyi K. Abegunde, Hong-Nan Sun, Fu-Ming Deng, and Miao Zhang. "Physicochemical characterization of enzymatically hydrolyzed heat treated granular starches." Starch - Stärke 65, no. 11-12 (November 2013): 893–901. http://dx.doi.org/10.1002/star.201200272.

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20

Ismailoglu, Sadiye Ozden, and Arzu Basman. "Physicochemical properties of infrared heat-moisture treated wheat starch." Starch - Stärke 68, no. 1-2 (September 18, 2015): 67–75. http://dx.doi.org/10.1002/star.201500160.

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21

Lope-Oter, Eva. "Maximum latent heat of neutron star matter without GR." EPJ Web of Conferences 258 (2022): 07007. http://dx.doi.org/10.1051/epjconf/202225807007.

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We show how the specific latent heat is relevant to characterize the first-order phase transitions in neutron stars. Our current knowledge of this dynamical quantity strongly depends on the uncertainty bands of Chiral Perturbation Theory and of pQCD calculations and can be used to diagnose progress on the equation of state. We state what is known to be hadron-model independent and without feedback from neutron star observations and, therefore, they can be used to test General Relativity as well as theories beyond GR, such as modified gravity.

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22

Lazzari, G., and F. V. De Blasio. "Specific heat of superfluid neutrons in neutron star crusts." Il Nuovo Cimento A 107, no. 8 (August 1994): 1423–26. http://dx.doi.org/10.1007/bf02775782.

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23

Wang, Yong Shuai, Jing Yang, Xiang Jun Yu, and Ke Li. "Temperature Field Analysis of High-Speed Gasoline Engine Cylinder Head Based on Fluid-Solid Coupling." Advanced Materials Research 680 (April 2013): 327–32. http://dx.doi.org/10.4028/www.scientific.net/amr.680.327.

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As the important part of the internal-combustion engine, cylinder head bears high thermal loads and mechanical loads. In order to analyse the merits or defects of cylinder head cooling system , built the 3-D model of cylinder head, and analysed the heat transfer processes between cylinder head and cooling water by fluid-solid coupled simulation in STAR-CCM+. The pressure nephograms and velocity vector of cooling water in the water jacket, and the whole temperature distributions of cylinder head were acquired. And analysed separately the temperature fields of fire power faces and exhaust passages which were under high heat loads .According to the analysis results , the structrue of cylinder head water jacket was evaluated and corresponding suggestions was put forward.

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24

Sednin, Alexei, Aliaksandr Mukhin, and Boris Balakin. "Use of vertical geothermal heat exchanger with nanofluid for heat supply systems." E3S Web of Conferences 288 (2021): 01089. http://dx.doi.org/10.1051/e3sconf/202128801089.

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Future district heating systems need to be more flexible and move towards a carbon-neutral generation. Compression heat pumps are foreseen to be promising future tools for district heating systems in EU countries. The paper presents the simulation data or a vertical double-pipe geothermal heat exchanger with ethylene glycol-Al2O3 as a working fluid. To simulate the operation of the heat exchanger, the STAR-CCM + CFD application was used. It has been determined the optimal volume particle concentrations of nanofluid and enhance of heat exchanger performance.

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25

Yakovlev, D. G., A. D. Kaminker, A. Y. Potekhin, and P. Haensel. "Model of heat diffusion in the outer crust of bursting neutron stars." Monthly Notices of the Royal Astronomical Society 500, no. 4 (November 15, 2020): 4491–505. http://dx.doi.org/10.1093/mnras/staa3547.

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ABSTRACT We study heat diffusion after an energy release in a deep spherical layer of the outer neutron star crust (107 ≲ ρ ≲ 4 × 1011 g cm−3). We demonstrate that this layer possesses specific heat-accumulating properties, absorbing heat and directing it mostly inside the star. It can absorb up to ∼1043–1044 erg due to its high heat capacity, until its temperature exceeds T ∼ 3 × 109 K and triggers a rapid neutrino cooling. A warm layer (T ∼ 108–3 × 109 K) can serve as a good heat reservoir, which is thermally decoupled from the inner crust and the stellar core for a few months. We present a toy model to explore the heat diffusion within the heat-accumulating layer, and we test this model using numerical simulations. We formulate some generic features of the heat propagation that can be useful, for instance, for the interpretation of superbursts in accreting neutron stars. We present a self-similar analysis of late afterglow after such superbursts, which can be helpful to estimate properties of bursting stars.

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26

Zhang, Chengli, Peng Wang, and Guoliang Song. "Performance Evaluation of STARPAM Polymer and Application in High Temperature and Salinity Reservoir." International Journal of Analytical Chemistry 2018 (December 18, 2018): 1–13. http://dx.doi.org/10.1155/2018/9653953.

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Based on the properties of high temperature and salinity reservoir, the water-soluble polymer with good heat resistance and salt tolerance can be obtained through copolymerization between 2-acrylamide-2-methyl sulfonate monomer (AMPSN) and acrylamide monomer (AM) in water. The star shaped stable complexes (STARPAM) with the star nucleus of β-CD are prepared by living radical polymerization, which can improve the viscosity and change the percolation characteristics of the polymer in porous media. In the article, the performance of the STARPAM (star-shaped polymer) with heat resistance and salt tolerance was evaluated by comparing the viscosification property, heat and salt resistance, calcium and magnesium tolerance, and long-term thermal stability of STARPAM (star-shaped polymer) with those of HPAM (partially hydrolyzed polyacrylamide) and MO-4000 (linear polymer). The results of physical simulation experiment showed that the viscosity of the STARPAM is 3.3 times that of MO-4000 and 4 times that of HPAM under the conditions of mineralization degree of 20000 mg/L, concentration of 1500 mg/L, and 75°C, which indicated that heat resistance and salt tolerance of the STARPAM are excellent. Oil displacement experiments showed that STARPAM can enhance oil recovery by 20.53% after water flooding, and the effect of oil displacement is excellent. At present, 19 wells were effective with a ratio of 95.2%. Compared with before treatment, the daily liquid production increased by 136 m3, daily oil production increased by 44.6 t, water cut decreased by 4.67 percentage points, and flow pressure decreased by 1.15 MPa.

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27

GHOSH, S. G., and D. W. DESHKAR. "NON-SPHERICAL COLLAPSE OF A RADIATING STAR." International Journal of Modern Physics D 12, no. 02 (February 2003): 317–23. http://dx.doi.org/10.1142/s0218271803002433.

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We study the junction conditions for non-spherical (plane symmetric) collapsing radiating star consisting of a shearing fluid undergoing radial heat flow with outgoing radiation. Radiation of the system is described by plane symmetric Vaidya solution. Physical quantities relating to the local conservation of momentum and surface red-shift are also obtained.

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28

Amézaga González, María Fernanda, Jazzely Acosta Bezada, Víctor Gómez Flores, Christian Chapa González, Jose Rurik Farias Mancilla, S. J. Castillo, Carlos Avila Orta, and Perla E. García-Casillas. "Effect of Physiological Fluid on the Photothermal Properties of Gold Nanostructured." International Journal of Molecular Sciences 24, no. 9 (May 6, 2023): 8339. http://dx.doi.org/10.3390/ijms24098339.

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Colloidal gold particles have been extensively studied for their potential in hyperthermia treatment due to their ability to become excited in the presence of an external laser. However, their light-to-heat efficiency is affected by the physiologic environment. In this study, we aimed to evaluate the ability of gold sphere, rod, and star-shaped colloids to elevate the temperature of blood plasma and breast cancer-simulated fluid under laser stimulation. Additionally, the dependence of optical properties and colloid stability of gold nanostructures with physiological medium, particle shape, and coating was determined. The light-to-heat efficiency of the gold particle is shape-dependent. The light-to-heat conversion efficiency of a star-shaped colloid is 36% higher than that of sphere-shaped colloids. However, the raised temperature of the surrounding medium is the lowest in the star-shaped colloid. When gold nanostructures are exited with a laser stimulation in a physiological fluid, the ions/cations attach to the surface of the gold particles, resulting in colloidal instability, which limits electron oscillation and diminishes the energy generated by the plasmonic excitation. Fluorescein (Fl) and polyethylene glycol (PEG) attached to gold spheres enhances their colloidal stability and light-to-heat efficiency; post-treatment, they remand their optical properties.

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29

Theander, O., and E. Westerlund. "Studies on Chemical Modifications in Heat-processed Starch and Wheat Flour." Starch - Stärke 39, no. 3 (1987): 88–93. http://dx.doi.org/10.1002/star.19870390306.

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30

Siljeström, M., I. Björck, and E. Westerlund. "Transglycosidation Reactions Following Heat Treatment of Starch – Effects on Enzymic Digestibility." Starch - Stärke 41, no. 3 (1989): 95–100. http://dx.doi.org/10.1002/star.19890410306.

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31

Abraham, T. Emilia. "Stabilization of Paste Viscosity of Cassava Starch by Heat Moisture Treatment." Starch - Stärke 45, no. 4 (1993): 131–35. http://dx.doi.org/10.1002/star.19930450404.

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32

Estes, John, Michael Kavic, Steven L. Liebling, Matthew Lippert, and John H. Simonetti. "Stability and observability of magnetic primordial black hole-neutron star collisions." Journal of Cosmology and Astroparticle Physics 2023, no. 06 (June 1, 2023): 017. http://dx.doi.org/10.1088/1475-7516/2023/06/017.

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Abstract The collision of a primordial black hole with a neutron star results in the black hole eventually consuming the entire neutron star. However, if the black hole is magnetically charged, and therefore stable against decay by Hawking radiation, the consequences can be quite different. Upon colliding with a neutron star, a magnetic black hole very rapidly comes to a stop. For large enough magnetic charge, we show that this collision can be detected as a sudden change in the rotation period of the neutron star, a glitch or anti-glitch.We argue that the magnetic primordial black hole, which then settles to the core of the neutron star, does not necessarily devour the entire neutron star; the system can instead reach a long-lived, quasi-stable equilibrium. Because the black hole is microscopic compared to the neutron star, most stellar properties remain unchanged compared to before the collision. However, the neutron star will heat up and its surface magnetic field could potentially change, both effects potentially observable.

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GOVENDER, M., K. P. REDDY, and S. D. MAHARAJ. "THE ROLE OF SHEAR IN DISSIPATIVE GRAVITATIONAL COLLAPSE." International Journal of Modern Physics D 23, no. 02 (January 29, 2014): 1450013. http://dx.doi.org/10.1142/s0218271814500138.

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In this paper, we investigate the physics of a radiating star undergoing dissipative collapse in the form of a radial heat flux. Our treatment clearly demonstrates how the presence of shear affects the collapse process; we are in a position to contrast the physical features of the collapsing sphere in the presence of shear with the shear-free case. By employing a causal heat transport equation of the Maxwell–Cattaneo form we show that the shear leads to an enhancement of the core temperature thus emphasizing that relaxational effects cannot be ignored when the star leaves hydrostatic equilibrium.

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34

Bejan, Adrian. "Every Snowflake is Not Unique." Mechanical Engineering 137, no. 01 (January 1, 2015): 40–41. http://dx.doi.org/10.1115/1.2015-jan-3.

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This article discusses various aspects of snowflake architectures. It is certain that every snowflake conforms to only one architecture: a flat star with six fishbones connected at the center. The latent heat of solidification, which is released by the water vapor that becomes solid at the bead surface. There comes a critical time when the spherical bead is no longer an efficient architecture for dissipating heat. The principle calls for design change, toward faster heat release and solidification. The growth of ice morphs abruptly into a ball continued in one plane by needles. Because of the configuration of the water molecule, the needles grow in six directions. The flat star transfers heat to the surroundings more easily than a spherical bead with the same diameter. In order to give credit to the view that every snowflake is unique, the actual configuration depends on many secondary effects, which are of random origin.

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35

Bošnjaković, Mladen, Simon Muhič, and Ante Čikić. "Experimental testing of the heat exchanger with star-shaped fins." International Journal of Heat and Mass Transfer 149 (March 2020): 119190. http://dx.doi.org/10.1016/j.ijheatmasstransfer.2019.119190.

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36

Kang, Shung-Wen, and Derlin Huang. "Fabrication of star grooves and rhombus grooves micro heat pipe." Journal of Micromechanics and Microengineering 12, no. 5 (June 21, 2002): 525–31. http://dx.doi.org/10.1088/0960-1317/12/5/303.

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37

Ootes, L. S., R. Wijnands, and D. Page. "Long-term temperature evolution of neutron stars undergoing episodic accretion outbursts." Astronomy & Astrophysics 630 (September 26, 2019): A95. http://dx.doi.org/10.1051/0004-6361/201936035.

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Context. Transient neutron star low-mass X-ray binaries undergo episodes of accretion, alternated with quiescent periods. During an accretion outburst, the neutron star heats up due to exothermic accretion-induced processes taking place in the crust. Besides the long-known deep crustal heating of nuclear origin, a likely non-nuclear source of heat, dubbed “shallow heating”, is present at lower densities. Most of the accretion-induced heat slowly diffuses into the core on a timescale of years. Over many outburst cycles, a state of equilibrium is reached when the core temperature is high enough that the heating and cooling (photon and neutrino emission) processes are in balance. Aims. We investigate how stellar characteristics and outburst properties affect the long-term temperature evolution of a transiently accreting neutron star. For the first time the effects of crustal properties are considered, particularly that of shallow heating. Methods. Using our code NSCool, we tracked the thermal evolution of a neutron star undergoing outbursts over a period of 105 yr. The outburst sequence is based on the regular outbursts observed from the neutron star transient Aql X-1. For each model we calculated the timescale over which equilibrium was reached and we present these timescales along with the temperature and luminosity parameters of the equilibrium state. Results. We performed several simulations with scaled outburst accretion rates, to vary the amount of heating over the outburst cycles. The results of these models show that the equilibrium core temperature follows a logarithmic decay function with the equilibrium timescale. Secondly, we find that shallow heating significantly contributes to the equilibrium state. Increasing its strength raises the equilibrium core temperature. We find that if deep crustal heating is replaced by shallow heating alone, the core would still heat up, reaching only a 2% lower equilibrium core temperature. Deep crustal heating may therefore not be vital to the heating of the core. Additionally, shallow heating can increase the quiescent luminosity to values higher than previously expected. The thermal conductivity in the envelope and crust, including the potentially low-conductivity pasta layer at the bottom of the crust, is unable to significantly alter the long-term internal temperature evolution. Stellar compactness and nucleon pairing in the core change the specific heat and the total neutrino emission rate as a function of temperature, with the consequences for the properties of the equilibrium state depending on the exact details of the assumed pairing models. The presence of direct Urca emission leads to the lowest equilibrium core temperature and the shortest equilibrium timescale.

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Yakovlev, D. G., and A. D. Kaminker. "Neutron Star Crusts With Magnetic Fields." International Astronomical Union Colloquium 147 (1994): 214–38. http://dx.doi.org/10.1017/s0252921100026385.

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AbstractThe properties of plasma in neutron star crusts with strong magnetic fields B = 1010 − 1013 G are reviewed: thermodynamic properties (equation of state, entropy, specific heat), transport properties (electron thermal and electrical conductivity of degenerate electron gas, radiative thermal conductivity of very surface nondegenerate layers) and neutrino energy losses. Classical effects of electron Larmor rotation in a magnetic field are considered as well as quantum effects of the electron motion (Landau levels). The influence of the magnetic fields on density and temperature profiles in the surface layers of neutron stars and on neutron star cooling is briefly discussed.

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Govender, M., A. Maharaj, Ksh Newton Singh, and Neeraj Pant. "Dissipative collapse of a Karmarkar star." Modern Physics Letters A 35, no. 20 (May 21, 2020): 2050164. http://dx.doi.org/10.1142/s0217732320501643.

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In this paper, we employ the Karmarkar condition to model a spherically symmetric radiating star undergoing dissipative gravitational collapse within the framework of classical general relativity. The collapse ensues from an initial static core satisfying the Karmarkar condition in isotropic coordinates and proceeds nonadiabatically by emitting energy in the form of a radial heat flux to the exterior Vaidya spacetime. We show that the dynamical nature of the collapse is sensitive to the initial static configuration that inherently links the embedding to the final remnant. Our model considered several physical tests on how an initially static stellar structure onset to a radiative collapse.

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Kaothekar, Sachin, and R. K. Chhajlani. "Effect of Radiative Heat-Loss Function and Finite Larmor Radius Corrections on Jeans Instability of Viscous Thermally Conducting Self-Gravitating Astrophysical Plasma." ISRN Astronomy and Astrophysics 2012 (September 29, 2012): 1–14. http://dx.doi.org/10.5402/2012/420938.

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The effect of radiative heat-loss function and finite ion Larmor radius (FLR) corrections on the self-gravitational instability of infinite homogeneous viscous plasma has been investigated incorporating the effects of thermal conductivity and finite electrical resistivity for the formation of a star in astrophysical plasma. The general dispersion relation is derived using the normal mode analysis method with the help of relevant linearized perturbation equations of the problem. Furthermore the wave propagation along and perpendicular to the direction of external magnetic field has been discussed. Stability of the medium is discussed by applying Routh Hurwitz’s criterion. We find that the presence of radiative heat-loss function and thermal conductivity modify the fundamental Jeans criterion of gravitational instability into radiative instability criterion. From the curves we see that temperature dependent heat-loss function, FLR corrections and viscosity have stabilizing effect, while density dependent heat-loss function has destabilizing effect on the growth rate of self-gravitational instability. Our result shows that the FLR corrections and radiative heat-loss functions affect the star formation.

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Pukkahuta, Chirdchan, and Saiyavit Varavinit. "Structural Transformation of Sago Starch by Heat-Moisture and Osmotic-Pressure Treatment." Starch - Stärke 59, no. 12 (December 2007): 624–31. http://dx.doi.org/10.1002/star.200700637.

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Watcharatewinkul, Yanika, Dudsadee Uttapap, Chureerat Puttanlek, and Vilai Rungsardthong. "Enzyme digestibility and acid/shear stability of heat-moisture treated canna starch." Starch - Stärke 62, no. 3-4 (April 2010): 205–16. http://dx.doi.org/10.1002/star.200900221.

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Pinto, Vânia Zanella, Nathan Levien Vanier, Bruna Klein, Elessandra da Rosa Zavareze, Moacir Cardoso Elias, Luiz Carlos Gutkoski, Elizabete Helbig, and Alvaro Renato Guerra Dias. "Physicochemical, crystallinity, pasting and thermal properties of heat-moisture-treated pinhão starch." Starch - Stärke 64, no. 11 (July 16, 2012): 855–63. http://dx.doi.org/10.1002/star.201200040.

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Ismailoglu, Sadiye Ozden, and Arzu Basman. "Effects of infrared heat-moisture treatment on physicochemical properties of corn starch." Starch - Stärke 67, no. 5-6 (March 23, 2015): 528–39. http://dx.doi.org/10.1002/star.201400266.

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Stute, Rolf. "Hydrothermal Modification of Starches: The Difference between Annealing and Heat/Moisture -Treatment." Starch - Stärke 44, no. 6 (1992): 205–14. http://dx.doi.org/10.1002/star.19920440603.

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Kawabata, Akiko, Naoaki Takase, Emako Miyoshi, Shigeru Sawayama, Toshiaki Kimura, and Kenichi Kudo. "Microscopic Observation and X-Ray Diffractometry of Heat/Moisture-Treated Starch Granules." Starch - Stärke 46, no. 12 (1994): 463–69. http://dx.doi.org/10.1002/star.19940461204.

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SKRIVER, ANNE, MARTIN B. HANSEN, and KARSTEN B. QVIST. "Image analysis applied to electron micrographs of stirred yogurt." Journal of Dairy Research 64, no. 1 (February 1997): 135–43. http://dx.doi.org/10.1017/s0022029996001884.

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An optimum or a high heat treatment of milk before yogurt preparation was applied according to an experimental design with the deliberate aim of making stirred yogurts with varying properties. Images of sections of yogurt samples were obtained using a transmission electron microscope. These were digitized and segmented via a threshold determination to separate the protein structure from the background. Four spatial statistical estimates were determined in order to evaluate their applicability for characterization of yogurt microstructure. The volume content was estimated and compared with the protein content obtained through chemical analysis. Heat treatment had no significant effect on volume content, as expected. The surface area of the protein aggregates was a useful measure to describe the difference between casein networks obtained by an optimum and a high heat treatment. The star volume gave a measure of the average local size of pores in the yogurt gel. The optimum heat treatment resulted in yogurt with small values for the star volume, indicating a less coarse structure of the casein network compared with yogurt prepared from high heat milk. The covariance function was able to differentiate between yogurts made using two types of heat treatment.

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Dai, Lixin, Jonathan C. McKinney, and M. Coleman Miller. "Energetic constraints on electromagnetic signals from double black hole mergers." Monthly Notices of the Royal Astronomical Society: Letters 470, no. 1 (May 31, 2017): L92—L96. http://dx.doi.org/10.1093/mnrasl/slx086.

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Abstract The possible Fermi detection of an electromagnetic counterpart to the double black hole merger GW150914 has inspired many theoretical models, some of which propose that the holes spiralled together inside a massive star. However, we show that the heat produced by the dynamical friction on such black hole orbits can exceed the stellar binding energy by a large factor, which means that this heat could destroy the star. The energy scale of the explosion and the terminal velocity of the gas can be much larger than those in conventional supernovae. If the star unbinds before the merger, it would be hard for enough gas to remain near the holes at the merger to produce a gamma-ray burst, and this consideration should be taken into account when models are proposed for electromagnetic counterparts to the coalescence of two stellar-mass black holes. We find that only when the two black holes form very close to the centre can the star certainly avoid destruction. In that case, dynamical friction can make the black holes coalesce faster than they would in vacuum, which leads to a modification of the gravitational waveform that is potentially observable by advanced LIGO.

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CHAN, R. "RADIATING GRAVITATIONAL COLLAPSE WITH SHEAR REVISITED." International Journal of Modern Physics D 12, no. 06 (July 2003): 1131–55. http://dx.doi.org/10.1142/s0218271803003463.

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A model is proposed for a collapsing radiating star consisting of a fluid with shear motion undergoing radial heat flow with outgoing radiation. The pressure of the star, at the beginning of the collapse, is isotropic but due to the presence of the shear motion of the fluid the pressure becomes more and more anisotropic. The radial and temporal behaviors of the density, the pressure, the total mass, the luminosity, the effective adiabatic index and the Kretschmann scalar are analyzed for a star with 6 M⊙. The final evolution is a star that radiates all its mass during the collapse, and thus, neither forming a black hole, as in the previous model, nor a naked singularity.

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Song, Xiuhuan, Hong Chi, Zibiao Li, Tianduo Li, and FuKe Wang. "Star-Shaped Crosslinker for Multifunctional Shape Memory Polyurethane." Polymers 12, no. 4 (March 26, 2020): 740. http://dx.doi.org/10.3390/polym12040740.

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Star-shaped cyclophosphazene (ACP) was employed as covalent crosslinker to form a rigid segment in polyurethanes network, to enhance the mechanical performance and to add extra flame retardant property. The effects of different ACP contents on the shape memory ability and fire resistance performance of polyurethane (PU) were studied. Tensile tests suggested high flexibility of the PUs with the maximum elongation-at-break of 161.59%. Dynamic mechanical analysis (DMA) indicated good shape recovery ratio of 72.58% after more than three repeated cycles. Under thermal treatment, the temporary shape could recover to its original state in 10 s. The peak heat release rate (pHRR), total heat released (THR) and temperature at pHRR (Tp) of flame-retardant shape memory polyurethane (FSPU) by micro-combustion calorimeter (MCC) was as low as 183.2 W/g, 21.4 KJ/g, 330.8 °C respectively, suggesting good inherent fire-resistant performance. As amine-containing crosslinkers are one of the most common building units in thermosetting polymers, we anticipate that our finding will have significant benefits beyond shape memory and fire-resistance.

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