Astrophysics and Space Science最新文献_第8页

Absolute emission height determination of the radio emission components of PSR B2111+46 at multiple bands by relativistic phase shift method 用相对论相移法测定多波段 PSR B2111+46 射电发射成分的绝对发射高度

IF 1.8 4区物理与天体物理

Astrophysics and Space Science Pub Date : 2024-08-28 DOI: 10.1007/s10509-024-04353-z

Tridib Roy, Mayuresh Surnis, Ramkrishna Das

{"title":"Absolute emission height determination of the radio emission components of PSR B2111+46 at multiple bands by relativistic phase shift method","authors":"Tridib Roy, Mayuresh Surnis, Ramkrishna Das","doi":"10.1007/s10509-024-04353-z","DOIUrl":"10.1007/s10509-024-04353-z","url":null,"abstract":"<div><p>Pulsars are believed to be one of the most important celestial objects in the universe. The emission mechanism of pulsars is still a big paradox for physicists, as no completely acceptable theory can reach a suitable consensus with observation. Some complicated coherent plasma processes and acceleration-based mechanisms in the pulsar magnetosphere generate a powerful radio beam. There have been dedicated theories such as the geometrical and relativistic phase shift (RPS) methods. The relativistic phase shift method is owing to the combined effects of aberration-retardation (A/R) and polar cap current effect (PCC), etc., and by implementing this method, we make quantitative inspections to deduce the emission altitude of the pulsar’s radio emission components. Here, we have shown the estimation of the emission height of pulsar PSR B2111+46 for both core and conal components at 925 MHz, 1.25 GHz, 1.65 GHz, and 4.85 GHz. Moreover, we have estimated the foot point, normalized with the last open field line constant, corresponding to pulse edges at multiple bands. Current analysis of the paper shows that at least for PSR B2111+46, the full polar cap is not sensitive to radio emission for most of the cases in the given stretch of radio frequency.</p></div>","PeriodicalId":8644,"journal":{"name":"Astrophysics and Space Science","volume":"369 8","pages":""},"PeriodicalIF":1.8,"publicationDate":"2024-08-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142175585","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

On the asymptotic persistence of Langmuir modes in kinematically complex plasma flows 论运动学复杂等离子体流中朗缪尔模式的渐近持续性

IF 1.8 4区物理与天体物理

Astrophysics and Space Science Pub Date : 2024-08-27 DOI: 10.1007/s10509-024-04355-x

Ketevan Arabuli, Andria Rogava, Stefaan Poedts

{"title":"On the asymptotic persistence of Langmuir modes in kinematically complex plasma flows","authors":"Ketevan Arabuli, Andria Rogava, Stefaan Poedts","doi":"10.1007/s10509-024-04355-x","DOIUrl":"10.1007/s10509-024-04355-x","url":null,"abstract":"<div><p>The dynamics of Langmuir modes, waves (LW), and shear Langmuir vortices (SLV) are studied in kinematically complex astrophysical plasma flows. It is found that they exhibit several peculiar, velocity shear-induced, <i>asymptotically persistent</i> phenomena, including efficient energy exchange with the background flow and various kinds of instabilities, leading to their exponential growth and echoing solutions with persistent wave-vortex-wave conversions. There is a remarkable similarity between these phenomena and those happening with compressible acoustic modes. The relevance and possible importance of these phenomena for different types of astrophysical plasma flow patterns with kinematic complexity are discussed. In particular, we argue that these physical processes may account for the persistent appearance of plasma oscillations in the heliosphere and interstellar plasma flows. In particular, we believe that the kinematically complex motion of plasma may naturally lead to the asymptotically persistent appearance of Langmuir modes that are born, grown, fed, sustained and maintained by these flows.</p></div>","PeriodicalId":8644,"journal":{"name":"Astrophysics and Space Science","volume":"369 8","pages":""},"PeriodicalIF":1.8,"publicationDate":"2024-08-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142175586","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Excess-entropy scaling in gravitational systems 引力系统中的超熵缩放

IF 1.8 4区物理与天体物理

Astrophysics and Space Science Pub Date : 2024-08-22 DOI: 10.1007/s10509-024-04354-y

Christine C. Dantas

引用次数: 0

Radio continuum emission from planetary nebulae in the Small Magellanic Cloud 小麦哲伦星云中行星状星云的射电连续波发射

IF 1.8 4区物理与天体物理

Astrophysics and Space Science Pub Date : 2024-08-14 DOI: 10.1007/s10509-024-04342-2

A. D. Asher, M. D. Filipović, I. Bojičić, R. Z. E. Alsaberi, E. J. Crawford, H. Leverenz

{"title":"Radio continuum emission from planetary nebulae in the Small Magellanic Cloud","authors":"A. D. Asher, M. D. Filipović, I. Bojičić, R. Z. E. Alsaberi, E. J. Crawford, H. Leverenz","doi":"10.1007/s10509-024-04342-2","DOIUrl":"10.1007/s10509-024-04342-2","url":null,"abstract":"<div><p>We report 11 new radio continuum measurements of established planetary nebulae (PNe) in the Small Magellanic Cloud (SMC) that we observed at 5.5 and 9 GHz with the Australia Telescope Compact Array (ATCA). These new radio detections are PNe with catalogued names: SMP SMC 2, SMP SMC 3, SMP SMC 5, SMP SMC 8, SMP SMC 13, SMP SMC 14, SMP SMC 19, MGPN SMC 8, SMP SMC 22, SMP SMC 26 and SMP SMC 27. We supplement our data with available high-resolution radio observations from MeerKAT and construct the spectral energy distribution (SED) in the radio regime for each PN. We determine the angular diameters of four of the eleven PNe from radio flux density alone using SED modelling, which are compared to the corresponding <i>Hubble Space Telescope</i> (HST) optical diameters. Our results are in good agreement with the optically-derived angular diameters from independent HST observations. We plot our new diameter estimates against a larger sample of Galactic PNe and compare diameters obtained via the SED method to those found in the literature. Our sample diameters, when compared to the Galactic PNe, suggest that the angular diameter measurement methods are comparable independent of the distance.</p></div>","PeriodicalId":8644,"journal":{"name":"Astrophysics and Space Science","volume":"369 8","pages":""},"PeriodicalIF":1.8,"publicationDate":"2024-08-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10509-024-04342-2.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142175589","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Correction to: Study on the time calibration method of the YangBaJing Hybrid Array 更正为杨八井混合阵列的时间校准方法研究

IF 1.8 4区物理与天体物理

Astrophysics and Space Science Pub Date : 2024-08-06 DOI: 10.1007/s10509-024-04348-w

Shaozhang Zhao, Tianlu Chen, Qi Gao, Youliang Feng

引用次数: 0

MHD lensing in inhomogeneous ISM for qualitative understanding of the morphology of supernova remnants 非均质 ISM 中的 MHD 透镜用于定性了解超新星残余的形态

IF 1.8 4区物理与天体物理

Astrophysics and Space Science Pub Date : 2024-08-06 DOI: 10.1007/s10509-024-04346-y

Yoshiaki Sofue

引用次数: 0

Correction to: Lateral density distributions of Cherenkov photons at different altitudes 更正：不同高度切伦科夫光子的侧向密度分布

IF 1.8 4区物理与天体物理

Astrophysics and Space Science Pub Date : 2024-08-05 DOI: 10.1007/s10509-024-04347-x

Xinlong Li, Tianlu Chen, Youliang Feng, Yangzhao Ren, Qingyuan Hou, Hengjiao Liu, Qingqian Zhou, Yaping Wang

引用次数: 0

Titanium oxide absorption as a proxy to detect long term variation and activity cycle in Proxima Centauri 以氧化钛吸收为替代物探测比邻星的长期变化和活动周期

IF 1.8 4区物理与天体物理

Astrophysics and Space Science Pub Date : 2024-08-02 DOI: 10.1007/s10509-024-04345-z

Fatemeh Azizi, Mohammad Taghi Mirtorabi, Rahimeh Foroughi

引用次数: 0

Interplay between neutrino kicks and hydrodynamic kicks of neutron stars and black holes 中子星和黑洞的中微子踢和流体动力踢之间的相互作用

IF 1.8 4区物理与天体物理

Astrophysics and Space Science Pub Date : 2024-08-02 DOI: 10.1007/s10509-024-04343-1

Hans-Thomas Janka, Daniel Kresse

{"title":"Interplay between neutrino kicks and hydrodynamic kicks of neutron stars and black holes","authors":"Hans-Thomas Janka, Daniel Kresse","doi":"10.1007/s10509-024-04343-1","DOIUrl":"10.1007/s10509-024-04343-1","url":null,"abstract":"<div><p>Neutron stars (NSs) are observed with high space velocities and elliptical orbits in binaries. The magnitude of these effects points to natal kicks that originate from asymmetries during the supernova (SN) explosions. Using a growing set of long-time 3D SN simulations with the <span>Prometheus-Vertex</span> code, we explore the interplay of NS kicks that are induced by asymmetric neutrino emission and by asymmetric mass ejection. Anisotropic neutrino emission can arise from a large-amplitude dipolar convection asymmetry inside the proto-NS (PNS) termed LESA (Lepton-number Emission Self-sustained Asymmetry) and from aspherical accretion downflows around the PNS, which can lead to anisotropic neutrino emission (absorption/scattering) with a neutrino-induced NS kick roughly opposite to (aligned with) the kick by asymmetric mass ejection. In massive progenitors, hydrodynamic kicks can reach up to more than 1300 km s<sup>−1</sup>, whereas our calculated neutrino kicks reach (55–140) km s<sup>−1</sup> (estimated upper bounds of (170–265) km s<sup>−1</sup>) and only ∼(10–50) km s<sup>−1</sup>, if LESA is the main cause of asymmetric neutrino emission. Therefore, hydrodynamic NS kicks dominate in explosions of high-mass progenitors, whereas LESA-induced neutrino kicks dominate for NSs born in low-energy SNe of the lowest-mass progenitors, when these explode nearly spherically. Our models suggest that the Crab pulsar with its velocity of ∼160 km s<sup>−1</sup>, if born in the low-energy explosion of a low-mass, single-star progenitor, should have received a hydrodynamic kick in a considerably asymmetric explosion. Black holes, if formed by the collapse of short-lived PNSs and solely kicked by anisotropic neutrino emission, obtain velocities of only some km s<sup>−1</sup>.</p></div>","PeriodicalId":8644,"journal":{"name":"Astrophysics and Space Science","volume":"369 8","pages":""},"PeriodicalIF":1.8,"publicationDate":"2024-08-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10509-024-04343-1.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141887249","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

A comparative study of solar activity parameters during the period 2009–2012 and 2020–2023 (ascending phase of solar cycles 24 and 25) 2009-2012年和2020-2023年（太阳周期24和25的上升阶段）太阳活动参数比较研究

IF 1.8 4区物理与天体物理

Astrophysics and Space Science Pub Date : 2024-08-02 DOI: 10.1007/s10509-024-04344-0

P. R. Singh, Upendra Kr. Singh Kushwaha

{"title":"A comparative study of solar activity parameters during the period 2009–2012 and 2020–2023 (ascending phase of solar cycles 24 and 25)","authors":"P. R. Singh, Upendra Kr. Singh Kushwaha","doi":"10.1007/s10509-024-04344-0","DOIUrl":"10.1007/s10509-024-04344-0","url":null,"abstract":"<div><p>In this paper, we performed solar synodic period (∼27 days) and heliospheric effect for selected solar activity parameters: sunspot number (SSN), sunspot area (SSA), modified coronal index (MCI), solar radio flux (F10.7), chromospheric composite Mg II index and Galactic cosmic rays (GCRs), during the ascending phase of solar cycles 24 and 25 (2009–2012 and 2020 to 2023). The Wavelet analyses of daily data of SSN, SSA, MCI, Mg II, and F10.7, reveal a solar rotational period of ∼27 days. The R Robper method is used to validate the observed periods; near one solar rotational period during the ascending phase of solar cycles 24 and 25. We observed cross-correlation and time lag for solar activity parameters (SSN, SSA, MCI, Mg II, and F10.7) with GCRs during the ascending phase of solar cycles 24 and 25 (2009–2012 and 2020 to 2023). We found the highest time lag for SSA is ∼300 days, and for SSN is ∼270 days during the ascending phase of solar cycle 25. We also found the highest cross-correlation values are 0.998 and 0.996 for chromospheric composite Mg II index with Galactic cosmic rays (GCRs) during the ascending phase of solar cycle 24 and 25 respectively. We found the chromospheric composite Mg II index is a good indicator of solar activity indices and it is strongly correlated to SSN.</p></div>","PeriodicalId":8644,"journal":{"name":"Astrophysics and Space Science","volume":"369 8","pages":""},"PeriodicalIF":1.8,"publicationDate":"2024-08-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141885326","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0