| 书目名称 | Neutron Stars and Pulsars | | 编辑 | Werner Becker | | 视频video | | | 概述 | Comprehensive reference written by leading international experts.Reviews historical development in pulsar research and presents current understanding and open questions.Includes supplementary material | | 丛书名称 | Astrophysics and Space Science Library | | 图书封面 |  | | 描述 | .Neutron stars are the most compact astronomical objects in the universe which are accessible by direct observation. Studying neutron stars means studying physics in regimes unattainable in any terrestrial laboratory. ..Understanding their observed complex phenomena requires a wide range of scientific disciplines, including the nuclear and condensed matter physics of very dense matter in neutron star interiors, plasma physics and quantum electrodynamics of magnetospheres, and the relativistic magneto-hydrodynamics of electron-positron pulsar winds interacting with some ambient medium. Not to mention the test bed neutron stars provide for general relativity theories, and their importance as potential sources of gravitational waves. It is this variety of disciplines which, among others, makes neutron star research so fascinating, not only for those who have been working in the field for many years but also for students and young scientists. ..The aim of this book is to serve as a reference work which not only reviews the progress made since the early days of pulsar astronomy, but especially focuses on questions such as: "What have we learned about the subject and how did we learn it? | | 出版日期 | Book 2009 | | 关键词 | Gravitational Waves from Spinning Neutron Stars; Gravity; Isolated Neutron Stars and Millisecond Pulsa | | 版次 | 1 | | doi | https://doi.org/10.1007/978-3-540-76965-1 | | isbn_softcover | 978-3-662-50104-7 | | isbn_ebook | 978-3-540-76965-1Series ISSN 0067-0057 Series E-ISSN 2214-7985 | | issn_series | 0067-0057 | | copyright | Springer-Verlag Berlin Heidelberg 2009 |
| 1 |
Front Matter |
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Abstract
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| 2 |
,Radio Pulsar Statistics, |
Duncan R. Lorimer |
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Abstract
Forty years after the discovery of radio pulsars by Jocelyn Bell and Antony Hewish at Cambridge in 1967 [22], the observed population presently exceeds 1,700 objects with spin periods in the range 1.4 ms to 8.5 s. Pulsar astronomy is currently enjoying a golden era, with over half of these discoveries in the past 7 years due largely to the phenomenal success of the Parkes multi beam survey [46]. From the sky distribution in Galactic coordinates shown in Fig. 1.1, it is immediately apparent that pulsars are concentrated strongly along the Galactic plane. This is particularly striking for the youngest pulsars known to be associated with supernova remnants. Also shown in Fig. 1.1 are the millisecond pulsars which have spin periods in the range 1.5–30 ms. The more isotropic sky distribution of the millisecond pulsars does not necessarily imply that they have a different spatial distribution; the difference simply reflects the observational bias against detecting short-period pulsars with increasing distance from the Sun. This is one of many selection effects that pervades the observed sample..From such a violent birth in supernovae, it is perhaps not surprising to learn that pulsars ar
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| 3 |
,Radio Emission Properties of Pulsars, |
Richard N. Manchester |
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Abstract
. Pulsar parameters used in this paper have been obtained from the ATNF Pulsar Catalogue, Version 1.29, http://www.atnf.csiro.au/research/pulsar/psrcat [44]. Pulsars are fascinating objects with a wide range of applications in physics and astronomy. Characterised observationally by a highly periodic pulse train with periodicities typically in the range a few milliseconds to several seconds, they are generally identified with highly magnetised and rapidly rotating neutron stars formed in supernova explosions. Rotation of the star causes beamed emission, probably emanating from open field lines associated with the magnetic poles, to sweep across the sky generating one observed pulse per rotation period. A total of 1,765 pulsars are now known and almost all of these lie within our Galaxy.. As Fig. 2.1 illustrates, pulsars come in two main classes, those with periods in the millisecond range and the so-called “normal” pulsars with periods of order 1 s. Most millisecond pulsars (MSPs) are binary, that is, in an orbit with another star, whereas only a few percent of normal pulsars are binary. MSPs, which comprise about 10% of the known population, are believed to be relatively old pulsa
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| 4 |
,Rotating Radio Transients, |
Maura McLaughlin |
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Abstract
Gamma-ray and X-ray telescopes have long been sensitive to transient phenomena, with rich scientific returns resulting from the discovery of sources such as gamma-ray bursts, soft gamma-ray repeaters and anomalous X-ray pulsars. The situation at radio wavelengths, however, is dramatically different. While radio telescopes typically have sensitivity to events with short timescales, they have much narrower fields of view than their high-energy counterparts. Consequently, most transient radio studies have been follow-up observations of events first detected at higher energies. Radio transient studies are important, however, as they can probe explosive and dynamic events which do not necessarily have counterparts at other wavelengths..Figure 3.1 illustrates the types of objects that we might expect to discover with surveys for short timescale (i.e. durations ≲ 1 day) radio transients. The brightest such sources are radio pulsars, with the “nano-giant” pulses from the Crab pulsar having brightness temperatures up to 10. K [23] and the single pulses of “normal” pulsars having brightness temperatures of 10. K. Well-known weaker sources include planetary radio flares [6], Type I and Type I
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| 5 |
,Intermittent Pulsars, |
Andrew G. Lyne |
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Abstract
Transient phenomena are usually difficult to find and characterise, particularly if much of the time is spent in a null state. This is true of two recently discovered types of transient radio source, namely the Rotating Radio Transient sources (RRATs) and the Intermittent Pulsars. Both spend much of their time invisible in quite different ways, and both have underlying periodicities which are attributable to rotating magnetic neutron stars. In these circumstances, they also represent the small tips of much larger populations which may cause us to revise our views of what “normal” neutron star behaviour is. RRATS are objects which emit occasional single pulses of radio emission, perhaps once every 100–1,000 rotation periods of the neutron star. The phenomenon is described in detail elsewhere in this volume [9]. The intermittent pulsars on the other hand behave like normal regular pulsars for intervals of time measured in days or years, with longer intervals when there is no emission at all. In this paper, we discuss the phenomenon, the search for other instances, the implications for pulsar magnetospheric physics and the galactic population of such objects.
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,The Double Pulsar: A Unique Lab for Relativistic Plasma Physics and Tests of General Relativity, |
Michael Kramer |
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Abstract
Almost a hundred years after Einstein formulated his theory of general relativity (GR), efforts in testing GR and its concepts are still being made by many colleagues around the world, using many different approaches. To date GR has passed all experimental and observational tests with flying colours, but in light of recent progress in observational cosmology in particular, the question of whether alternative theories of gravity need to be considered is as topical as ever..Many experiments are designed to achieve ever more stringent tests by either increasing the precision of the tests or by testing different, new aspects. Some of the most stringent tests are obtained by satellite experiments in the solar system, providing exciting limits on the validity of GR and alternative theories of gravity like tensor-scalar theories. However, solar-system experiments are made in the gravitational weak-field regime, while deviations from GR may appear only in strong gravitational fields. It happens that nature provides us with an almost perfect laboratory to test the strong-field regime using binary radio pulsars.
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,X-Ray Emission from Pulsars and Neutron Stars, |
Werner Becker |
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Abstract
The idea of . stars can be traced back to the early 1930s, when Subrahmanyan Chandrasekhar discovered that there is no way for a collapsed stellar core with a mass more than 1.4 times the solar mass, M, to hold itself up against gravity once its nuclear fuel is exhausted. This implies that a star left with M › 1.4 M (the .) would keep collapsing and eventually disappear from view..After the discovery of the neutron by James Chadwick in 1932 scientists speculated on the possible existence of a ., which would have a radius of the order ofR 3x 10. cm. In view of the peculiar stellar parameters, Lev Landau called these objects “unheimliche Sterne“ (weird stars), expecting that they would never be observed because of their small size and expected low optical luminosity.
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| 8 |
,Isolated Neutron Stars: The Challenge of Simplicity, |
Roberto Turolla |
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Abstract
The seven soft, thermal sources discovered by ROSAT offer an unprecedented opportunity to unveil the temperature and magnetic field surface distribution of isolated neutron stars. This makes a direct measurement of the star radius and mass within reach and will allow to place tight constraints on matter equation of state at nuclear densities. In this chapter the main observational properties of the . are reviewed, and the current status of theoretical modeling presented. Emphasis is placed on the main challenge these objects pose to theorists, namely how can a cooling neutron star emit a nearly perfect blackbody spectrum. Open issues concern the origin of the broad absorption features (or lack thereof) detected around a few hundred electron volts, the search for new candidates and the (possible) links of the Magnificent Seven with other classes of Galactic neutron star sources, the newly discovered rotating radio transients and the magnetar candidates in particular..First hypothesised in the 1930s, neutron stars have been for more than 40 years a theoretician‘s dainty, until the discovery of the first radio pulsar [27]. Since then, neutron stars have been mostly detected at radio w
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,Millisecond Pulsars in Globular Clusters and the Field, |
Jonathan E. Grindlay,Slavko Bogdanov |
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Abstract
Globular clusters are preferred for the study of millisecond pulsars (MSPs), given the 蠙100 increase in their number per unit stellar mass than in the Galaxy at large. X-ray observations of globulars with imaging grazing incidence telescopes have proven to be at least as sensitive as radio telescopes for MSP detection and spectral classification, but not (yet) for period discovery due to the relatively low count rates. However, for known periods, pulse-phase spectroscopy studies are remarkably effective. We provide an initial overview of the current X-ray studies of MSPs in globular clusters as well as in the Galaxy field. Early X-ray studies of MSPs with ., and . are reviewed briefly and put into the context of current results. Globular clusters observed with the . X-ray Observatory, given its exceptional angular resolution, have clarified the range of MSP types (thermal vs. non-thermal) and overall populations. Observations of several nearby field MSPs with ., with its temporal-spectral resolution, have given new measurements of the M/R (compactness) of neutron stars from precise measures of their soft X-ray pulse profiles as a function of energy. X-ray spectral-timing of MSPs ca
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| 10 |
,Theory of Radiative Transfer in Neutron Star Atmospheres and Its Applications, |
Vyacheslav E. Zavlin |
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Abstract
Before the first neutron star was discovered in 1967 as a radio pulsar. by Jocelyn Bell [22] it had been predicted that neutron stars can be powerful sources of thermal X-ray emission, having surface temperatures of about one million Kelvin [11, 78]. This prediction and the discovery of the first pulsar became one of many motivations for further developing X-ray astronomy at the end of the 1950s. Observational study of thermal radiation from neutron stars began in 1978 with the launch of the Einstein observatory which detected X-ray emission in the 0.2—4 keV range from a number of neutron stars and neutron star candidates. The ROSAT mission which was sensitive in the 0.1—2.4 keV range marks the beginning of the “decade of space science”, which in the 1990s provided many important results on observing X-ray emission from neutron stars. By extending the energy range up to 10 keV ASCA and BeppoSAX added important information on the pulsar emission in the harder band pass whereas EUVE and HST allowed to study neutron stars in the very soft 0.07—0.2 keV and optical/UV bands. More details on results from observations of neutron stars can be found in the Chaps. 6—8. New excellent observat
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| 11 |
,Neutron Star Interiors and the Equation of State of Superdense Matter, |
Fridolin Weber,Rodrigo Negreiros,Philip Rosenfield |
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Abstract
Neutron stars contain matter in one of the densest forms found in the Universe. This feature, together with the unprecedented progress in observational astrophysics, makes such stars superb astrophysical laboratories for a broad range of exciting physical studies. This paper gives an overview of the phases of dense matter predicted to make their appearance in the cores of neutron stars. Particular emphasis is put on the role of strangeness. Net strangeness is carried by hyperons, K-mesons, H-dibaryons, and strange quark matter, and may leave its mark in the masses, radii, moment of inertia, dragging of local inertial frames, cooling behavior, surface composition, and the spin evolution of neutron stars. These observables play a key role for the exploration of the phase diagram of dense nuclear matter at high baryon number density but low temperature, which is not accessible to relativistic heavy ion collision experiments.
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| 12 |
,Neutron Star Cooling: I, |
Dany Page |
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Abstract
This chapter presents a basic, but detailed, introduction to the physical and astro-physical issues involved in the study of the thermal evolution of isolated neutron stars. Results of numerical calculations,. for both minimal and enhanced cooling scenarios, are presented and compared with observational data..The first conjectures about the possible existence of stellar neutron cores by Landau [37] and Baade and Zwicky [6] and the pioneering work of Oppenheimer and Volkoff [48] pointed to very mysterious, exotic, small and dense objects. Forty years after the actual discovery of neutron stars [28] these early thoughts have been fully confirmed: neutron stars are demonstrably very small and dense, they very probably enclose some exotic form(s) of matter, and they are still mysterious..
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| 13 |
,Neutron Star Cooling: II, |
Sachiko Tsuruta |
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Abstract
It was more than 70 years ago when Baade and Zwicky [3] speculated that an “exotic” star consisting mostly of neutrons, now known as a neutron star, may be formed when a normal star collapses through a supernova explosion. During the subsequent years in the 1930s several theorists, including Oppenheimer and Volkoff [35], discussed the properties of neutron stars. However, it was not until the late 1950s to the early 1960s, when curiosity on such a hypothetical object revived [11,73]. As far as I am aware Cameron [11] is the first author who discussed thermodynamic problems of neutron stars. This article‘s author chose to explore this problem as one of the projects on neutron stars as her PhD thesis [59]. The research started as a purely theoretical endeavor, but before the calculations were completed we learned of the discovery of the first Galactic X-ray source Sco X-1, which was soon followed by the second such Galactic X-ray source detection, this time in the Crab supernova remnant [15]. It was immediately suggested by several theorists [19, 59, 66] that these strong X-ray sources might be neutron stars, because if these X-rays are blackbody radiation as expected, the radius of
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| 14 |
,Turning Points in the Evolution of Isolated Neutron Stars’Magnetic Fields, |
Ulrich Geppert |
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Abstract
During the life of isolated neutron stars (NSs) their magnetic field passes through a variety of evolutionary phases. Depending on its strength and structure and on the physical state of the NS (e.g., cooling, rotation), the field looks qualitatively and quantitatively different after each of these phases. Three of them, the phase of MHD instabilities immediately after NS‘s birth, the phase of fallback which may take place hours to months after NS‘s birth, and the phase when strong temperature gradients may drive thermoelectric instabilities, are concentrated in a period lasting from the end of the proto-NS phase until 100, perhaps 1,000 years, when the NS has become almost isothermal. The further evolution of the magnetic field proceeds in general inconspicuous since the star is in isolation. However, as soon as the product of Larmor frequency and electron relaxation time, the so-called magnetization parameter (ω. .), locally and/or temporally considerably exceeds unity, phases, also unstable ones, of dramatic changes of the field structure and magnitude can appear..The energy of the magnetic fields of neutron stars is even for magnetar field strengths (̃10. G) negligible in compa
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| 15 |
,Pulsar Spin, Magnetic Fields, and Glitches, |
Malvin Ruderman |
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Abstract
As the number of nucleons in stable atomic nuclei increases, their neutron to proton ratios grow larger. So does the fraction of each atom‘s electrons which is contained within its nuclear volume. If an atomic weight (A) were to exceed 10. that atom would resemble a canonical neutron star: a huge nucleus consisting mainly of neutrons, several percent protons, and an electron cloud almost entirely contained within the nucleus. In the commonly observed nuclei this limit cannot be reached because nucleon-nucleon attractive forces can no longer prevent nuclear fission from Coulomb repulsion when A exceeds 300. However, if A were to reach 10., gravitational attraction would become sufficiently strong to hold the star together and we can have a stable conventional neutron star. In it, the dominant neutron sea is a quantum fluid with properties very similar to those of very low temperature superfluid Helium. The much less abundant protons form a superconductor whose properties closely resemble those of a BCS (Bardeen, Cooper, Schrieffer) electron superconductor. Both of these quantum fluids are well understood and their expected properties confirmed in laboratory experiments. Most astroph
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| 16 |
,Pulsar Emission: Where to Go, |
Jonathan Arons |
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Abstract
Pulsars are the quintessential dogs that don‘t bark in the night — their observed loss of rotational energy mostly disappears into the surrounding world while leaving few traces of that energy loss in observable photon emission. They are the prime example of compact objects which clearly lose their energy through a large scale Poynting flux..In this chapter I survey recent successes in the application of relativistic MHD and force-free electrodynamics to the modeling of the pulsars rotational energy loss mechanism as well as to the structure and emission characteristics of Pulsar Wind Nebulae. I suggest that unsteady reconnection in the current sheet separating the closed from the open zones of the magnetosphere is responsible for the torque fluctuations observed in some pulsars, as well as for departures of the braking index from the canonical value of 3. I also discuss the theory of high energy pulsed emission from these neutron stars, emphasizing the significance of the boundary layer between the closed and open zones as the active site in the outer magnetosphere. I elaborate on the conflict between the models currently in use to interpret the gamma-ray and X-ray pulses from the
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| 17 |
,The Theory of Pulsar Winds and Nebulae, |
John G. Kirk,Yuri Lyubarsky,Jerome Petri |
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Abstract
The theory of pulsar winds and the nebulae they energize is currently celebrating its golden jubilee. Ten years before the discovery of pulsars it was already apparent that the magnetic field and relativistic particles that produce the radiation of the Crab Nebula must have their origin in a central stellar object [104]. Today, about 50 similarly powered objects are known, and some of them, like the Crab, are detected and even resolved at all accessible photon frequencies, from the radio to TeV gamma-rays. The rotation of the central neutron star [98] is now universally accepted as the energy source fuelling these objects, but the details of the coupling mechanism are still unclear. In this article we review current theoretical ideas on this subject and their relationship to observations. We concentrate on the magneto-hydrodynamic description of the relativistic outflow driven by the pulsar and on the bubble it inflates in the surrounding medium..The discussion is organised as follows: in Sect. 16.2 we consider the region between the surface of the neutron star and the . a surface of cylindrical radius .L = . /(2π), where . is the pulsar period. The speed of an object that co-rotat
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| 18 |
,Implications of HESS Observations of Pulsar, |
Ocker C. de Jager,Arache Djannati-Ataï |
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Abstract
Even before the discovery of pulsars, pulsar wind nebulae (PWN) like the Crab Nebula were identified as belonging to a class of cosmic radio sources with rela-tivistic electrons moving in magnetized plasmas to give the continuum radiation as observed. Visionaries like [36] already predicted that we should be able to measure the magnetic field strength in PWN using the combination of synchrotron and inverse Compton (IC) radiation. Following this, [43] were the first to provide us with a sophisticated one dimensional (1D) magneto hydrodynamical models (MHD) model of the Crab Nebula, which predicted a magnetic field strength distribution, consistent with broadband multi-wavelength (radio through very high energy gamma-ray) constraints [12,25, 39]..The discovery of the Crab pulsar in 1968 confirmed suspicions that a rapidly spinning neutron star should provide the energy input into the Crab Nebula, but soon questions concerning the spin-down of pulsars in relation to the evolution of the nebulae arose. Whereas a few Crab-like remnants were discovered, Vela X, assumed to be associated with the 11,000 year old Vela pulsar, raised the question about the evolution of PWN as described by [6
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| 19 |
,High Energy Emission from Pulsars and Pulsar Wind Nebulae, |
Kwong Sang Cheng |
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Abstract
Pulsars are accidentally discovered by the Cambridge scientists [48]. Shortly thereafter, Gold [39] and Pacini [72] proposed that pulsars are rotating neutron stars with surface magnetic fields of around 10. G. Gold [39] pointed out that such objects could account for many of the observed features of pulsars, such as the remarkable stability of the pulsar period, and predicted a small increase in the period as the pulsar slowly lost rotational energy. With the discovery of the Vela pulsar with a period of 88 ms [65], the identification of the Crab pulsar with a period of 33 ms [86] and the discovery of slowdown of Crab pulsar [77], it was essentially confirmed that pulsars are rapidly rotating neutron stars. So far, over 1,500 radio pulsars have been found (see the most updated list of pulsars in www.atnf.csiro.au/research/pulsar/). The radio luminosities of these pulsars are small compared with the energy loss rate due to the pulsar spin down (̃10.−10−.). Strong high-frequency radiation in the X-ray band has been observed from about two dozens pulsars (for recent review cf. [6, 7]), but only eight pulsars have been confirmed to emit high energy γ-rays (cf. [94] for a recent review
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| 20 |
,High-energy Emission from the Polar Cap and Slot Gap, |
Alice K. Harding |
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Abstract
Forty years after the discovery of rotation-powered pulsars, we still do not understand many aspects of their pulsed emission. In the last few years there have been some fundamental developments in acceleration and emission models. In this Chapter I will review both the basic physics of the models as well as the latest developments in understanding the high-energy emission of rotation-powered pulsars, with particular emphasis on the polar-cap and slot-gap models. Special and general relativistic effects play important roles in pulsar emission, from inertial frame-dragging near the stellar surface to aberration, time-of-flight and retardation of the magnetic field near the light cylinder. Understanding how these effects determine what we observe at different wavelengths is critical to unraveling the emission physics..Rotation-powered pulsars are fascinating astrophysical sources and excellent laboratories for study of fundamental physics of strong gravity, strong magnetic fields, high densities and relativity. The major advantage we have in studying pulsars is that we know they are rotating neutron stars and that they derive their power from rotational energy loss. The challenge is
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发表于 2025-3-21 18:03:38
