Log in

Relevant bibliographies by topics / Starquake / Journal articles

Journal articles on the topic 'Starquake'

To see the other types of publications on this topic, follow the link: Starquake.

Author: Grafiati

Published: 9 March 2023

Last updated: 10 March 2023

Create a spot-on reference in APA, MLA, Chicago, Harvard, and other styles

Select a source type:

Consult the top 39 journal articles for your research on the topic 'Starquake.'

Next to every source in the list of references, there is an 'Add to bibliography' button. Press on it, and we will generate automatically the bibliographic reference to the chosen work in the citation style you need: APA, MLA, Harvard, Chicago, Vancouver, etc.

You can also download the full text of the academic publication as pdf and read online its abstract whenever available in the metadata.

Browse journal articles on a wide variety of disciplines and organise your bibliography correctly.

1

Li, Hui-Quan, and Jian-Cheng Wang. "Transient Phenomena from Gas Erupting Neutron Stars." Research in Astronomy and Astrophysics 22, no. 1 (January 1, 2022): 015017. http://dx.doi.org/10.1088/1674-4527/ac3899.

Full text

Abstract:

Abstract Starquakes probably occur in rapidly spinning or ultra high field neutron stars. In this article, we argue that highly compressed gas containing electron–positron pairs could evaporate and erupt from inside the neutron star when a crack forms and then heals during a starquake. Under the influence of the existing oscillation modes of the star, the crack may have sufficiently large size and long lifetime. An appropriate amount of gas can erupt into the magnetosphere with relativistic and nearly uniform velocity, producing various transient and bursting phenomena.

APA, Harvard, Vancouver, ISO, and other styles

2

TELESCA, LUCIANO. "QUANTIFYING THE TIME-CLUSTERING IN SGR1806-20 BURSTS." Fluctuation and Noise Letters 05, no. 03 (September 2005): L417—L422. http://dx.doi.org/10.1142/s0219477505002847.

Full text

Abstract:

The time-clustering behavior of the neutron star SGR1806-20 burst sequence (detected by the International Cometary Explorer, ICE) has been analyzed. The presence of two different timescaling regions, related to the "foreshock" and "aftershock" phases, separated by the largest event occurred on November 16, 1983, 8:34 GMT, E = 5.17 · 1041 erg , has been evidenced. The results highlight that starquake foreshocks involve medium timescales from about 30 minutes to approximately 5 days, while starquake aftershocks involve longer timescales ranging up 4 months.

APA, Harvard, Vancouver, ISO, and other styles

3

Wang, Weiyang, Rui Luo, Han Yue, Xuelei Chen, Kejia Lee, and Renxin Xu. "FRB 121102: A Starquake-induced Repeater?" Astrophysical Journal 852, no. 2 (January 16, 2018): 140. http://dx.doi.org/10.3847/1538-4357/aaa025.

Full text

APA, Harvard, Vancouver, ISO, and other styles

4

Bond, P. "Cluster and Double Star see massive 'starquake'." Astronomy & Geophysics 46, no. 6 (December 1, 2005): 6.5—a—6.5. http://dx.doi.org/10.1093/astrog/46.6.6.5-a.

Full text

APA, Harvard, Vancouver, ISO, and other styles

5

Blaes, O., R. Blandford, P. Goldreich, and P. Madau. "Neutron starquake models for gamma-ray bursts." Astrophysical Journal 343 (August 1989): 839. http://dx.doi.org/10.1086/167754.

Full text

APA, Harvard, Vancouver, ISO, and other styles

6

Negi, P. S. "A starquake model for the Vela pulsar." Monthly Notices of the Royal Astronomical Society 366, no. 1 (February 11, 2006): 73–78. http://dx.doi.org/10.1111/j.1365-2966.2005.09735.x.

Full text

APA, Harvard, Vancouver, ISO, and other styles

7

Kiss, Mózsi. "Starquake ends hiatus in soft X-ray polarimetry." Nature Astronomy 4, no. 5 (May 2020): 450–51. http://dx.doi.org/10.1038/s41550-020-1105-4.

Full text

APA, Harvard, Vancouver, ISO, and other styles

8

Link, Bennett, Lucia M. Franco, and Richard I. Epstein. "Starquake‐induced Magnetic Field and Torque Evolution in Neutron Stars." Astrophysical Journal 508, no. 2 (December 1998): 838–43. http://dx.doi.org/10.1086/306457.

Full text

APA, Harvard, Vancouver, ISO, and other styles

9

Giliberti, E., and G. Cambiotti. "Starquakes in millisecond pulsars and gravitational waves emission." Monthly Notices of the Royal Astronomical Society 511, no. 3 (January 29, 2022): 3365–76. http://dx.doi.org/10.1093/mnras/stac245.

Full text

Abstract:

ABSTRACT So far, only transient gravitational waves (GWs) produced by catastrophic events of extra-galactic origin have been detected. However, it is generally believed that there should be also continuous sources of GWs within our Galaxy, such as accreting neutron stars (NSs), that could in principle be detected in the next near future. In fact, in these objects, centrifugal forces can be so strong to break the NS crust (causing a starquake), thus producing a quadrupole moment responsible for the continuous emission of GWs. At equilibrium, the angular momentum gained by accretion and the one lost via GWs emission should balance each other, stopping the stellar spin-up. We hereinafter investigate the above physical picture within the framework of a Newtonian model describing compressible, non-magnetized, and self-gravitating NSs. In particular, we calculate the rotational frequency need to break the stellar crust of an accreting pulsar and we estimate the upper limit for the ellipticity due to this event. We find that the maximum starquake-induced ellipticity ranges from 10−9 to 10−5, depending on the stellar mass and its equation of state. The corresponding equilibrium frequency that we calculate is in good agreement with observations and, for all the scenarios, it is below the higher NS frequency observed of 716.36 Hz. Finally, we also discuss possible observational constraints on the ellipticity upper limit of accreting pulsars.

APA, Harvard, Vancouver, ISO, and other styles

10

HORVATH, J. E. "DETECTABILITY OF GRAVITATIONAL WAVE BURSTS FROM A CLASS OF NEUTRON STAR STARQUAKE GRB MODELS." International Journal of Modern Physics D 05, no. 01 (February 1996): 35–43. http://dx.doi.org/10.1142/s0218271896000047.

Full text

Abstract:

A large class of gamma-ray burst (GRB) models (overwhelming until recently) involve-the release of energy in a neutron star quake. Even though the extreme isotropy of the GRB sky established by the BATSE experiment has now shifted the interest to cosmological models, the former starquake scenarios are still attractive and may naturally produce a gravitational wave burst which carries most of the released energy. We discuss the prospects for detection of these high-frequency bursts by the forthcoming interferometers and spheroidal antennas, emphasizing the most recent results on the distribution and nature of the GRB sources. We find that, even if the overall picture is correct, the positive detection of GRB-associated gravitational wave bursts is unlikely and therefore these events will not be a prime target for the detectors.

APA, Harvard, Vancouver, ISO, and other styles

11

Negi, P. S. "Neutron star sequences and the starquake glitch model for the Crab and the Vela pulsars." Astrophysics and Space Science 332, no. 1 (October 16, 2010): 145–53. http://dx.doi.org/10.1007/s10509-010-0501-0.

Full text

APA, Harvard, Vancouver, ISO, and other styles

12

BASTRUKOV, S., I. MOLODTSOVA, J. YANG, and V. PAPOYAN. "PULSATING NEUTRON STAR AS A SOURCE OF QUASISTATIC WAVES OF GRAVITY IN INTERSTELLAR MEDIUM." International Journal of Modern Physics A 20, no. 32 (December 30, 2005): 7593–602. http://dx.doi.org/10.1142/s0217751x05025425.

Full text

Abstract:

The hydrodynamic waves of gravity in the galactic interstellar medium generated by a pulsating neutron star are discussed in this paper. It is shown that the frequency of oscillations of interstellar gas–dust matter in this wave is proportional to that for the g-mode in the neutron star bulk. The corresponding periods are of the millisecond duration. The collective oscillations of charged species in the interstellar wave of gravity can produce electromagnetic radiation, and that the only radio waves of this radiation can freely travel through the galactic gas–dust clouds, suggests that this kind of interstellar waves can manifest itself in the radio range of spectra of a neutron star undergoing pulsations triggered by starquake. This inference is in line with the statement that quasiperiodic micropulses with a time scale of a few milliseconds located in the windows of the main pulse train of the radio pulsar spectra owe their origin to pulsations of neutron stars.

APA, Harvard, Vancouver, ISO, and other styles

13

Takatsuka, T., and R. Tamagaki. "Postglitch Timing Behavior of Vela and Crab Pulsars in an Extended Starquake Model for Neutron Stars with Pion-Condensed Core." Progress of Theoretical Physics 82, no. 5 (November 1, 1989): 945–64. http://dx.doi.org/10.1143/ptp.82.945.

Full text

APA, Harvard, Vancouver, ISO, and other styles

14

Bisnovatyi-Kogan, G. S., and A. F. Illarionov. "Low Energy Lines in Spectra of Gamma Bursts." International Astronomical Union Colloquium 115 (1990): 63–69. http://dx.doi.org/10.1017/s0252921100012148.

Full text

Abstract:

AbstractWe connect the phenomenon of gamma ray bursts with nuclear explosions on the old neutron stars. The matter of the neutron star in the non-equilibrium layer at depths of 30 m ≤ h ≥ 100 m consists of superheavy (A ≥ 300) nuclei with a surplus of neutrons (A/Z = 3 ÷ 4). These nuclei are metastable and exist only at high pressure. After the starquake some of the matter from non-equilibrium layer may move upwards and its nuclei become unstable. The β-decay is followed by a chain reaction of fission and nuclear explosion. The gamma ray burst is observed as radiation of the star surface heated to high temperature. Some mass may be ejected, forming expanding cloud. It consists mainly of the iron Fe56 with small (≤ 1%) additions of heavy elements (Ba, I, …) arising from the fission. The passage of stellar gamma radiation through the expanding plasma clouds leads to the formation of short-lived spectral features. Strong absorption of the soft gamma rays on K-electrons of Fe56 must be observed in the early stages. The gamma quanta with energies ε = 40–70 keV beyond the K-edge of the heavy elements (Ba, I, …) are absorbed in the later stages. A wide Kα line (εα = 30 keV) appears simultaneously. The free-free emission of expanding hot plasma cloud may be observed as a short flash in optical band.

APA, Harvard, Vancouver, ISO, and other styles

15

Wang, W. H., X. Y. Lai, E. P. Zhou, J. G. Lu, X. P. Zheng, and R. X. Xu. "Pulsar glitches in a strangeon star model. II. The activity." Monthly Notices of the Royal Astronomical Society 500, no. 4 (November 12, 2020): 5336–49. http://dx.doi.org/10.1093/mnras/staa3520.

Full text

Abstract:

ABSTRACT Glitch is supposed to be a useful probe into pulsar’s interior, but the underlying physics remains puzzling. The glitch activity may reflect a lower limit of the crustal moment of inertia in conventional neutron star models. Nevertheless, its statistical feature could also be reproduced in the strangeon star model, which is focused here. We formulate the glitch activity of normal radio pulsars under the framework of starquake of solid strangeon star model, the shear modulus of strangeon matter is constrained to be $\mu \simeq 3\times 10^{34}~\rm erg\,cm^{-3}$, consistent with previous work. Nevertheless, about ten times the shift in oblateness accumulated during glitch interval is needed to fulfill the statistical observations. The fact that typical glitch sizes of two rapidly evolving pulsars (the Crab pulsar and PSR B0540-69) are about two orders of magnitude lower than that of the Vela pulsar, significantly lower than the oblateness change they can supply, indicates probably that only a part of oblateness change is relieved when a pulsar is young. The unreleased oblateness and stress may relax as compensation in the following evolution. The small glitch sizes and low glitch activity of the Crab pulsar can be explained simultaneously in this phenomenological model. Finally, we obtain energy release to be $\Delta E\sim 2.4\times 10^{40}~\rm erg$ and $\Delta E\sim 4.2\times 10^{41}~\rm erg$ for typical glitch size of Δν/ν ∼ 10−6 (Vela-like) and ∼10−8 (Crab-like). The upcoming SKA may test this model through the energy release and the power-law relation between the reduced recovery coefficient $Q/|\dot{\nu }|^{1/2}$ and Δν/ν.

APA, Harvard, Vancouver, ISO, and other styles

16

Kosovichev, Alexander G. "Sunquakes and starquakes." Proceedings of the International Astronomical Union 9, S301 (August 2013): 349–52. http://dx.doi.org/10.1017/s1743921313014579.

Full text

Abstract:

AbstractIn addition to well-known mechanisms of excitation of solar and stellar oscillations by turbulent convection and instabilities, the oscillations can be excited by an impulsive localized force caused by the energy release in solar and stellar flares. Such oscillations have been observed on the Sun (‘sunquakes’), and created a lot of interesting discussions about physical mechanisms of the impulsive excitation and their relationship to the flare physics. The observation and theory have shown that most of a sunquake's energy is released in high-degree, high-frequency p modes. In addition, there have been reports on helioseismic observations of low-degree modes excited by strong solar flares. Much more powerful flares observed on other stars can cause ‘starquakes’ of substantially higher amplitude. Observations of such oscillations can provide new asteroseismic information and also constraints on mechanisms of stellar flares. I discuss the basic properties of sunquakes, and initial attempts to detect flare-excited oscillations in Kepler short-cadence data.

APA, Harvard, Vancouver, ISO, and other styles

17

Rowan, L. "ASTROPHYSICS: Observing Starquakes." Science 298, no. 5597 (November 15, 2002): 1303a—1303. http://dx.doi.org/10.1126/science.298.5597.1303a.

Full text

APA, Harvard, Vancouver, ISO, and other styles

18

Kurtz, Don, Simon Jeffrey, and Conny Aerts. "Starquakes spring stellar surprises." Astronomy & Geophysics 57, no. 4 (July 19, 2016): 4.37–4.42. http://dx.doi.org/10.1093/astrogeo/atw151.

Full text

APA, Harvard, Vancouver, ISO, and other styles

19

Franco, L. M., B. Link, and R. I. Epstein. "Starquakes in Neutron Stars." Symposium - International Astronomical Union 195 (2000): 391–92. http://dx.doi.org/10.1017/s0074180900163235.

Full text

Abstract:

The Crab and other pulsars suffer sudden and permanent increases in their spin-down rates in association with glitches, suggesting that the external torque on these objects grows in steps. Here, we describe how torque changes may arise from starquakes, occurring as the star spins down and its rigid crust becomes less oblate. We study the evolution of strain in the crust, the initiation of starquakes, the effects on the magnetic field geometry, and possible observable consequences for neutron star spin down. We find that the stellar crust begins breaking at the rotational equator, forming a fault inclined at an angle to the equator and directed toward the magnetic poles. The resulting asymmetric matter redistribution produces a misalignment of the angular momentum and spin axes. Subsequently, damped precession to a new rotational state increases the angle between rotation and magnetic axes. The change in this angle could increase the external torque, producing a permanent increase in the spin-down rate.

APA, Harvard, Vancouver, ISO, and other styles

20

Joss, Paul C. "Starquakes and γ-ray bursts." Nature 349, no. 6305 (January 1991): 103–4. http://dx.doi.org/10.1038/349103a0.

Full text

APA, Harvard, Vancouver, ISO, and other styles

21

Middleditch, J., F. E. Marshall, Q. D. Wang, E. V. Gotthelf, and W. Zhang. "Predicting the Starquakes in PSR J0537−6910." Astrophysical Journal 652, no. 2 (December 2006): 1531–46. http://dx.doi.org/10.1086/508736.

Full text

APA, Harvard, Vancouver, ISO, and other styles

22

Whyte, Chelsea. "Mystery space signals could come from starquakes." New Scientist 244, no. 3251 (October 2019): 15. http://dx.doi.org/10.1016/s0262-4079(19)31900-1.

Full text

APA, Harvard, Vancouver, ISO, and other styles

23

Bedding, T. R., H. Kjeldsen, I. K. Baldry, F. Bouchy, R. P. Butler, F. Carrier, F. Kienzle, G. W. Marcy, S. J. O’Toole, and C. G. Tinney. "Solar-Like Oscillations in β Hydri: Evidence for Short-Lived High-Amplitude Oscillations." International Astronomical Union Colloquium 185 (2002): 464–67. http://dx.doi.org/10.1017/s025292110001681x.

Full text

Abstract:

AbstractVelocity measurements of the G2 subgiant β Hyi with both UCLES and CORALIE show a clear excess of power centred at 1.0 mHz. In the UCLES data we find evidence for a short-lived, high-amplitude oscillation event. If confirmed as a feature of subgiants, such ‘starquakes’ would make it harder to measure accurate mode frequencies and perform asteroseismology.

APA, Harvard, Vancouver, ISO, and other styles

24

Keer, L., and D. I. Jones. "Developing a model for neutron star oscillations following starquakes." Monthly Notices of the Royal Astronomical Society 446, no. 1 (November 13, 2014): 865–91. http://dx.doi.org/10.1093/mnras/stu2123.

Full text

APA, Harvard, Vancouver, ISO, and other styles

25

Bisnovatyi-Kogan, G. S. "Theory of Gamma Ray Bursters." Symposium - International Astronomical Union 125 (1987): 501–19. http://dx.doi.org/10.1017/s0074180900161273.

Full text

Abstract:

Gamma ray bursters are interpreted as nuclear explosions under the surface of neutron stars. The explosions occur after transportation of the matter with nonequilibrium composition during starquakes in outer layers where the matter becomes unstable and explodes as a result of a developing chain reaction. In the nonequilibrium matter nuclear charge Z decreases with increasing density, contrary to the equilibrium composition. Formation of a shock wave and total energy output are calculated. Parameters of the mighty burst of 5 March 1979 are estimated. Formation of observed lines in different partions of the range and a possible nature of accompanying optical bursts are discussed with the proposed model as a basis.

APA, Harvard, Vancouver, ISO, and other styles

26

Wang, Wei-Hua, Heng Xu, Wei-Yang Wang, Shuang Du, Quan Cheng, Xiao-Ping Zheng, and Ren-Xin Xu. "Constraining mechanism associated with fast radio burst and glitch from SGR J1935." Monthly Notices of the Royal Astronomical Society 507, no. 2 (July 31, 2021): 2208–19. http://dx.doi.org/10.1093/mnras/stab2213.

Full text

Abstract:

ABSTRACT The discovery of fast radio burst (FRB) 200428 from galactic SGR J1935+2154 makes it possible to measure rotational changes accompanied by FRBs and to test several FRB models which may be simultaneously associated with glitches. Inspired by this idea, we present order of magnitude calculations to the scenarios proposed. FRB models such as global starquakes, crust fractures, and collisions between pulsars and asteroids/comets are discussed. For each mechanism, the maximum glitch sizes are constrained by the isotropic energy release during the X-ray burst and/or the SGR J1935+2154-like radio burst rate. Brief calculations show that, the maximum glitch sizes for different mechanisms differ by order(s) of magnitude. If glitches are detected to be coincident with FRBs from galactic magnetars in the future, glitch behaviours (such as glitch size, rise time-scale, the recovery coefficient, and spin-down rate offset) are promising to serve as criterions to distinguish glitch mechanisms and in turn to constrain FRB models.

APA, Harvard, Vancouver, ISO, and other styles

27

Kapiris, P. G., G. T. Balasis, J. A. Kopanas, G. N. Antonopoulos, A. S. Peratzakis, and K. A. Eftaxias. "Scaling similarities of multiple fracturing of solid materials." Nonlinear Processes in Geophysics 11, no. 1 (February 25, 2004): 137–51. http://dx.doi.org/10.5194/npg-11-137-2004.

Full text

Abstract:

Abstract. It has recently reported that electromagnetic flashes of low-energy -rays emitted during multi-fracturing on a neutron star, and electromagnetic pulses emitted in the laboratory by a disordered material subjected to an increasing external load, share distinctive statistical properties with earthquakes, such as power-law energy distributions (Cheng et al., 1996; Kossobokov et al., 2000; Rabinovitch et al., 2001; Sornette and Helmstetter, 2002). The neutron starquakes may release strain energies up to erg, while, the fractures in laboratory samples release strain energies approximately a fraction of an erg. An earthquake fault region can build up strain energy up to approximately erg for the strongest earthquakes. Clear sequences of kilohertz-megahertz electromagnetic avalanches have been detected from a few days up to a few hours prior to recent destructive earthquakes in Greece. A question that arises effortlessly is if the pre-seismic electromagnetic fluctuations also share the same statistical properties. Our study justifies a positive answer. Our analysis also reveals "symptoms" of a transition to the main rupture common with earthquake sequences and acoustic emission pulses observed during laboratory experiments (Maes et al., 1998).

APA, Harvard, Vancouver, ISO, and other styles

28

Leonard, Thomas, Orestis Papasouliotis, and Ian G. Main. "A Poisson model for identifying characteristic size effects in frequency data: Application to frequency-size distributions for global earthquakes, “starquakes”, and fault lengths." Journal of Geophysical Research: Solid Earth 106, B7 (July 10, 2001): 13473–84. http://dx.doi.org/10.1029/2000jb900429.

Full text

APA, Harvard, Vancouver, ISO, and other styles

29

Lu, Ruipeng, Han Yue, Xiaoyu Lai, Weihua Wang, Shenjian Zhang, and Renxin Xu. "Quakes of Compact Stars." Monthly Notices of the Royal Astronomical Society, January 25, 2023. http://dx.doi.org/10.1093/mnras/stad270.

Full text

Abstract:

Abstract Glitches are commonly observed for pulsars, which are explained by various mechanisms. One hypothesis attributes the glitch effect to the instantaneous moment of inertia change of the whole star caused by a starquake, which is similar to earthquakes caused by fast dislocation occurring on planar faults for the static stress, though the quake-induced dynamics responsible for glitch (superfluid vortex vs. pure starquake) remains still unknown. However, a theoretical model to quantitatively explain the stress loading, types of starquakes, and co-seismic change of moment of inertia is rarely discussed. In this study, we incorporate elastic deformation theories of earthquakes into the starquake problems. We compute the field of stress loading associated with rotation deceleration and determine the optimal type of starquakes at various locations. Two types of pulsar structure models, i.e. neutron and strangeon star models, are included in the computation and their differences are notable. Our calculation shows that the observed glitch amplitude can be explained by the starquakes in the strangeon star model, though the required scaled starquake magnitude is much larger than that occurred on the Earth. We further discuss the possibility to compute the energy budget and other glitch phenomena using the starquake model in the elastic medium framework.

APA, Harvard, Vancouver, ISO, and other styles

30

Wright, Katherine. "Starquake Observations Near Their Teenage Years." Physics 14 (January 21, 2021). http://dx.doi.org/10.1103/physics.14.9.

Full text

APA, Harvard, Vancouver, ISO, and other styles

31

Giliberti, E., G. Cambiotti, M. Antonelli, and P. M. Pizzochero. "Modelling strains and stresses in continuously stratified rotating neutron stars." Monthly Notices of the Royal Astronomical Society, November 5, 2019. http://dx.doi.org/10.1093/mnras/stz3099.

Full text

Abstract:

Abstract We introduce a Newtonian model for the deformations of a compressible, auto-gravitating and continuously stratified neutron star. The present framework can be applied to a number of astrophysical scenarios as it allows to account for a great variety of loading forces. In this first analysis, the model is used to study the impact of a frozen adiabatic index in the estimate of rotation-induced deformations: we assume a polytropic equation of state for the matter at equilibrium but, since chemical reactions may be slow, the perturbations with respect to the unstressed configuration are modeled by using a different adiabatic index. We quantify the impact of a departure of the adiabatic index from its equilibrium value on the stressed stellar configuration and we find that a small perturbation can cause large variations both in displacements and strains. As a first practical application, we estimate the strain developed between two large glitches in the Vela pulsar showing that, starting from an initial unstressed configuration, it is not possible to reach the breaking threshold of the crust, namely to trigger a starquake. In this sense, the hypothesis that starquakes could trigger the unpinning of superfluid vortices is challenged and, for the quake to be a possible trigger, the solid crust must never fully relax after a glitch, making the sequence of starquakes in a neutron star an history-dependent process.

APA, Harvard, Vancouver, ISO, and other styles

32

Gibney, Elizabeth. "Mysterious radiowave blast may have come from starquake." Nature, December 2, 2015. http://dx.doi.org/10.1038/nature.2015.18935.

Full text

APA, Harvard, Vancouver, ISO, and other styles

33

"Kepler spots starquakes." Astronomy & Geophysics 51, no. 6 (November 30, 2010): 6.10. http://dx.doi.org/10.1111/j.1468-4004.2010.51609_8.x.

Full text

APA, Harvard, Vancouver, ISO, and other styles

34

"News. To the ends of the spectrum; To leap or not leap?; Stripes on Mars; Massive 'starquake'; Giant eye opens in Namibia; How did Halley align churches?; With geomagnetism, probably; Secret seismology." Astronomy and Geophysics 46, no. 6 (December 2005): 6.04–6.06. http://dx.doi.org/10.1111/j.1468-4004.2005.46604.x.

Full text

APA, Harvard, Vancouver, ISO, and other styles

35

Brumfiel, Geoff. "Starquakes Rock an Ion Crystal." Focus 8 (October 2001). http://dx.doi.org/10.1103/physrevfocus.8.23.

Full text

APA, Harvard, Vancouver, ISO, and other styles

36

Rencoret, J. A., C. Aguilera-Gómez, and A. Reisenegger. "Revisiting neutron starquakes caused by spin-down." Astronomy & Astrophysics, August 2, 2021. http://dx.doi.org/10.1051/0004-6361/202141499.

Full text

APA, Harvard, Vancouver, ISO, and other styles

37

Contadakis, M. E., S. J. Avgoloupis, and Ch Papantoniou. "Detection of starquakes on the flare star AD Leo." Astronomische Nachrichten, July 3, 2017. http://dx.doi.org/10.1002/asna.201713307.

Full text

APA, Harvard, Vancouver, ISO, and other styles

38

Sornette, D., and A. Helmstetter. "Occurrence of Finite-Time Singularities in Epidemic Models of Rupture, Earthquakes, and Starquakes." Physical Review Letters 89, no. 15 (September 20, 2002). http://dx.doi.org/10.1103/physrevlett.89.158501.

Full text

APA, Harvard, Vancouver, ISO, and other styles

39

Zhang, Zhao Joseph, Bin-Bin Zhang, and Yan-Zhi Meng. "A Comptonized Fireball Bubble: Physical Origin of Magnetar Giant Flares." Monthly Notices of the Royal Astronomical Society, February 9, 2023. http://dx.doi.org/10.1093/mnras/stad443.

Full text

Abstract:

Abstract Magnetar Giant Flares (MGFs) have been long proposed to contribute at least a sub-sample of the observed short Gamma-ray Bursts (GRBs). The recent discovery of the short GRB 200415A in the nearby galaxy NGC 253 established a textbook-version connection between these two phenomena. Unlike previous observations of the Galactic MGFs, the unsaturated instrument spectra of GRB 200415A provide for the first time an opportunity to test the theoretical models with the observed γ-ray photons. This paper proposed a new readily fit-able model for the MGFs, which invokes an expanding fireball Comptonized by the relativistic magnetar wind at photosphere radius. In this model, a large amount of energy is released from the magnetar crust due to the magnetic reconnection or the starquakes of the star surface and is injected into confined field lines, forming a trapped fireball bubble. After breaking through the shackles and expanding to the photospheric radius, the thermal photons of the fireball are eventually Comptonized by the relativistic e± pairs in the magnetar wind region, which produces additional higher-energy gamma-ray emission. The model predicts a modified thermal-like spectrum characterized by a low-energy component in the Rayleigh-Jeans regime, a smooth component affected by coherent Compton scattering in the intermediate energy range, and a high-energy tail due to the inverse Compton process. By performing a Monte-Carlo fit to the observational spectra of GRB 200415A, we found that the observation of the burst is entirely consistent with our model predictions.

APA, Harvard, Vancouver, ISO, and other styles

We offer discounts on all premium plans for authors whose works are included in thematic literature selections. Contact us to get a unique promo code!