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Correlation Between Radio Loudness and the Eddington Ratio in Quasars

IF 1.1 4区物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS

Astronomische Nachrichten

Pub Date : 2024-11-04 DOI: 10.1002/asna.20240072

Jing-Jing Shen, Xiang-Tao Zeng, Wei-Rong Huang, Ze-Yuan Tang, Jun-Hui Fan

Quasars can be categorized into radio-loud and radio-quiet populations based on radio properties. The physical mechanisms underlying this dichotomy have long been an active area of investigation. In this work, we analyze multi-wavelength data from 851 quasars matched between the SDSS DR14 and FIRST catalogs, requiring emission line measurements with signal-to-noise ratios > 3, we fit quasar optical continuum spectra and compute the radio loudness, luminosities, and Eddington ratios. We classify quasars as radio-loud or radio-quiet using a dividing line of $� � � \log � �_{L � � 6 � cm � �} � = � - � 2.7 � \log � R � + � 44.3 � � �$ . We find that the distribution of the Eddington ratio and radio luminosity is different between the radio-loud and radio-quiet quasars, and the correlation between the Eddington ratio and radio loudness is disparate as well. The Eddington ratio shows a weakly positive correlation with radio loudness in both the whole sample and radio-loud quasars, which imply that the Eddington ratio contributes to the radio loudness but it is not the dominant factor and that additional factors influence relativistic jet production in radio-loud quasars. However, the Eddington ratio is anti-correlated with radio loudness in radio-quiet quasars, potentially related to the properties of the accretion disk.

根据射电特性，类星体可分为射电响和射电静两种。长期以来，这种二分法的物理机制一直是一个活跃的研究领域。在这项工作中，我们分析了与 SDSS DR14 和 FIRST 星表匹配的 851 个类星体的多波长数据，要求测量信噪比为 > 3 的发射线，拟合类星体的光学连续谱，并计算射电响度、光度和爱丁顿比。我们用 log L 6 cm = - 2.7 log R + 44.3 $$ log {L}_{6mathrm{cm}}=-2.7log R+44.3 $$ 的分界线把类星体分为射电响度大和射电安静两种。我们发现，在射电噪声大的类星体和射电噪声小的类星体之间，埃丁顿比和射电光度的分布是不同的，埃丁顿比和射电噪声之间的相关性也是不同的。在整个样本和射电噪声大的类星体中，埃丁顿比值与射电响度呈弱正相关，这意味着埃丁顿比值对射电响度有影响，但不是主要因素，射电噪声大的类星体中还有其他因素影响相对论射流的产生。然而，在射电安静的类星体中，埃丁顿比与射电响度是反相关的，这可能与吸积盘的特性有关。

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引用次数: 0

Editor's Note: The X-Ray Mysteries of Neutron Stars and White Dwarfs

IF 1.1 4区物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS

Astronomische Nachrichten

Pub Date : 2024-10-27 DOI: 10.1002/asna.20240093

Norbert Schartel

引用次数: 0

Probing the Propeller Regime With Wide Neutron Star Binaries

IF 1.1 4区物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS

Astronomische Nachrichten

Pub Date : 2024-10-27 DOI: 10.1002/asna.20240096

M. D. Afonina, S. B. Popov

We model the duration of the propeller stage in wide binary systems with neutron stars and calculate the time of accretion onset for various propeller models. We apply our modeling to the symbiotic X-ray binary SWIFT J0850.8-4219. Unless a propeller with a very slow spin-down is operating, it is very improbable to find a system similar to SWIFT J0850.8-4219 at the propeller stage. Then we model the evolution of a neutron star in a binary with a solar-like companion. We calculate for which orbital separations and magnetic fields a neutron star can start to accrete while the companion is still on the Main sequence. We demonstrate that for the magnetic field $� � � B � ≲ � �^{10 � 12 �} � � �$ G neutron stars at the orbital separation $� � � a � ≳ � 1 � � �$ AU do not reach the propeller stage. In the case of a slow propeller spin-down, neutron stars never start to accrete. For the more rapid propeller spin-down, a neutron star can start to accrete or spend a long time at the propeller stage depending on the parameters.

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引用次数: 0

Issue Information: Astron. Nachr. 07/2024 发行信息：Astron.Nachr.07/2024

IF 1.1 4区物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS

Astronomische Nachrichten

Pub Date : 2024-10-15 DOI: 10.1002/asna.20249007

引用次数: 0

Cover Picture: Astron. Nachr. 8/2024 封面图片：Astron.Nachr.8/2024

IF 1.1 4区物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS

Astronomische Nachrichten

Pub Date : 2024-10-15 DOI: 10.1002/asna.20249016

Hikmet Çakmak, Talar Yontan, Selçuk Bilir, Timothy S. Banks, Raúl Michel, Esin Soydugan, Seliz Koç, Hülya Erçay

Vector-Point Diagrams (left panels) and proper-motion component vectors (right panels) for identified member stars in the open clusters Ruprecht 1 and Ruprecht 171. These two previously little-studied open clusters, both at a distance of approximately 1.5 kpc, have been characterized and studied in some detail in the related paper by Çakmak and collaborators, published in this issue e240054.

开放星团 Ruprecht 1 和 Ruprecht 171 中已识别成员星的矢量点图（左图）和正运动分量矢量（右图）。Çakmak及其合作者在本期e240054上发表的相关论文对这两个以前很少研究的疏散星团进行了详细的描述和研究。

引用次数: 0

Denoising Medium Resolution Stellar Spectra With Neural Networks

IF 1.1 4区物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS

Astronomische Nachrichten

Pub Date : 2024-10-10 DOI: 10.1002/asna.20240049

Balázs Pál, László Dobos

We trained denoiser autoencoding neural networks on medium resolution simulated optical spectra of late-type stars to demonstrate that the reconstruction of the original flux is possible at a typical relative error of a fraction of a percent down to a typical signal-to-noise ratio of $� � � 10 � � �$ per pixel. We show that relatively simple networks are capable of learning the characteristics of stellar spectra while still flexible enough to adapt to different values of extinction and fluxing imperfections that modifies the overall shape of the continuum, as well as to different values of Doppler shift. Denoised spectra can be used to find initial values for traditional stellar template fitting algorithms and—since evaluation of pretrained neural networks is significantly faster than traditional template fitting—denoiser networks can be useful when a fast analysis of the noisy spectrum is necessary, for example during observations, between individual exposures.

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引用次数: 0

HX Velorum: Ellipsoidal/Rotational Binary With β Cep Type Component HX Velorum带有 β Cep 型成分的椭球/旋转双星

IF 1.1 4区物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS

Astronomische Nachrichten

Pub Date : 2024-10-08 DOI: 10.1002/asna.20240028

B. Gürol

<div> We present the Transiting Exoplanet Survey Satellite (TESS) light curve analysis of HX Velorum, located in the Southern Hemisphere, where one of the components is found for the first time to be a <math> <semantics> <mrow> <mi>β</mi> </mrow> <annotation>$$ beta $$</annotation> </semantics></math> Cep (BCEP) type pulsator. The TESS observations of HX Velorum were published in a total of 6 sectors. Fourier analysis of the observations reveals that the frequencies can be divided into two categories, one of which is related to the orbital period and the other related to the <math> <semantics> <mrow> <mi>β</mi> </mrow> <annotation>$$ beta $$</annotation> </semantics></math> Cep-type pulsation. Its non-eclipsing light curve was analyzed with the well-known Wilson–Devinney code, and we obtained the geometric and physical parameters of the components using published radial velocity and light curve data by making some assumptions. We obtained plausible masses and radii of the primary and secondary components as <math> <semantics> <mrow> <msub> <mi>M</mi> <mn>1</mn> </msub> <mo>=</mo> <mn>9.48</mn> <mo>±</mo> <mn>0.27</mn> <msub> <mi>M</mi> <mo>⊙</mo> </msub> </mrow> <annotation>$$ {M}_1=9.48pm 0.27{M}_{odot } $$</annotation> </semantics></math>, <math> <semantics> <mrow> <msub> <mi>M</mi> <mn>2</mn> </msub> <mo>=</mo> <mn>5.92</mn> <mo>±</mo> <mn>0.17</mn> <msub> <mi>M</mi> <mo>⊙</mo> </msub> </mrow> <annotation>$$ {M}_2=5.92pm 0.17{M}_{odot } $$</annotation> </semantics></math> and <math> <semantics> <mrow> <msub> <mi>R</mi> <mn>1</mn> </msub> <mo>=</mo> <mn>3.93</mn> <mo>±</mo> <mn>0.04</mn> <msub> <mi>R</mi> <mo>⊙</mo> </msub> </mrow> <annotation>$$ {R}_1=3.93pm 0.04{R}_{odot } $$</annotation> </semantics></math>, <math> <semantics> <mrow> <msub>

我们展示了 Transiting Exoplanet Survey Satellite（TESS）对位于南半球的 HX Velorum 星的光变曲线分析，首次发现其中的一个成分是一个 β$ beta$ Cep（BCEP）型脉动器。TESS 对 HX Velorum 的观测共发布了 6 个扇区。对观测数据的傅立叶分析表明，其频率可分为两类，一类与轨道周期有关，另一类与 β $ beta $ Cep 型脉动有关。我们用著名的威尔逊-德文尼（Wilson-Devinney）代码分析了它的非彗星光曲线，并通过一些假设，利用已公布的径向速度和光曲线数据，获得了各组成部分的几何和物理参数。我们得到的主、副成分的质量和半径分别为 M 1 = 9.48 ± 0.27 M ⊙ $$ {M}_1=9.48pm 0.27{M}_{odot }$ ，M 2 = 5.48 ± 0.27 M ⊙ $$ {M}_1=9.48pm 0.27{M}_{odot }$ 。$$ , M 2 = 5.92 ± 0.17 M ⊙ $ $ {M}_2=5.92pm 0.17{M}_{odot }$ 和 R 1 = 3.92 ± 0.17 M ⊙ $ {M}_2=5.92pm 0.17{M}_{odot }$ 。$$ 和 R 1 = 3.93 ± 0.04 R ⊙ $$ {R}_1=3.93pm 0.04{R}_{odot }.$$ , R 2 = 3.59 ± 0.03 R ⊙ $$ {R}_2=3.59pm 0.03{R}_{odot }.分别为 $$ 。得到的系统距离为 ∼ 400 $ sim 400 $ pc，小于文献中发现的盖亚距离。

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引用次数: 0

Red Quasars: Estimation of SMBH Spin, Mass, and Accretion Disk Inclination Angle 红色类星体估计SMBH自旋、质量和吸积盘倾角

IF 1.1 4区物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS

Astronomische Nachrichten

Pub Date : 2024-10-06 DOI: 10.1002/asna.20240058

M. Yu. Piotrovich, S. D. Buliga, T. M. Natsvlishvili

We estimated values of spin, mass, and inclination angle for sample of 42 red quasars. Our estimations show that two objects: F2MS J1113+1244 and F2MS J1434+0935 with the highest Eddington ratios may have geometrically thick disk. Six objects: SDSS J0036-0113, S82X 0040+0058, S82X 0118+0018, S82X 0303-0115, FBQS J1227+3214, S82X 2328-0028 may have “retrograde” rotation. Analysis of estimated spin values shows that red quasar population may contain Seyfert galaxies and NLS1.

我们估算了 42 个红色类星体样本的自旋、质量和倾角值。我们的估算结果表明，有两个天体爱丁顿比值最高的两个天体：F2MS J1113+1244 和 F2MS J1434+0935，可能具有几何厚度的圆盘。六个天体SDSS J0036-0113、S82X 0040+0058、S82X 0118+0018、S82X 0303-0115、FBQS J1227+3214、S82X 2328-0028可能存在 "逆行 "旋转。对估计自旋值的分析表明，红色类星体群中可能包含赛弗星系和 NLS1。

引用次数: 0

Photometric and Kinematic Studies of Open Clusters Ruprecht 1 and Ruprecht 171 开放星团 Ruprecht 1 和 Ruprecht 171 的光度和运动学研究

IF 1.1 4区物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS

Astronomische Nachrichten

Pub Date : 2024-10-03 DOI: 10.1002/asna.20240054

Hikmet Çakmak, Talar Yontan, Selçuk Bilir, Timothy S. Banks, Raúl Michel, Esin Soydugan, Seliz Koç, Hülya Erçay

<div> This study outlines a detailed investigation using CCD UBV and Gaia DR3 data sets of the two open clusters Ruprecht 1 (Rup-1) and Ruprecht 171 (Rup-171). Fundamental astrophysical parameters such as color excesses, photometric metallicities, ages, and isochrone distances were based on UBV-data analyses, whereas membership probability calculations, structural and astrophysical parameters, as well as the kinematic analyses were based on Gaia DR3-data. We identified 74 and 596 stars as the most probable cluster members with membership probabilities over 50% for Rup-1 and Rup-171, respectively. The color excesses <math> <semantics> <mrow> <mi>E</mi> <mrow> <mo>(</mo> <mrow> <mi>B</mi> <mo>−</mo> <mi>V</mi> </mrow> <mo>)</mo> </mrow> </mrow> <annotation>$$ Eleft(B-Vright) $$</annotation> </semantics></math> were obtained as <math> <semantics> <mrow> <mn>0.166</mn> <mo>±</mo> <mn>0.022</mn> </mrow> <annotation>$$ 0.166pm 0.022 $$</annotation> </semantics></math> and <math> <semantics> <mrow> <mn>0.301</mn> <mo>±</mo> <mn>0.027</mn> </mrow> <annotation>$$ 0.301pm 0.027 $$</annotation> </semantics></math> mag for Rup-1 and Rup-171, respectively. Photometric metallicity analyses were performed by considering F-G type main-sequence member stars and found to be <math> <semantics> <mrow> <mrow> <mo>[</mo> <mrow> <mi>Fe</mi> <mo>/</mo> <mi>H</mi> </mrow> <mo>]</mo> </mrow> <mo>=</mo> <mo>−</mo> <mn>0.09</mn> <mo>±</mo> <mn>0.16</mn> </mrow> <annotation>$$ left[mathrm{Fe}/mathrm{H}right]=-0.09pm 0.16 $$</annotation> </semantics></math> and <math> <semantics> <mrow> <mrow> <mo>[</mo> <mrow> <mi>Fe</mi> <mo>/</mo> <mi>H</mi> </mrow> <mo>]</mo> </mrow> <mo>=</mo> <mo>−</mo> <mn>0.20</mn> <mo>±</mo>

本研究利用 CCD UBV 和 Gaia DR3 数据集对两个疏散星团 Ruprecht 1（Rup-1）和 Ruprecht 171（Rup-171）进行了详细调查。基本天体物理参数，如颜色过量、光度金属性、年龄和等时距离等，都是基于 UBV 数据分析的，而成员概率计算、结构和天体物理参数以及运动学分析则是基于 Gaia DR3 数据。我们分别为 Rup-1 和 Rup-171 确定了 74 和 596 颗恒星为最可能的星团成员，其成员概率超过 50%。Rup-1和Rup-171的颜色过量E ( B - V ) $$ Eleft(B-Vright) $$ 分别为0.166 ± 0.022 $$ 0.166pm 0.022 $$ 和 0.301 ± 0.027 $$ 0.301pm 0.027 $$ mag。通过对F-G型主序成员星进行光度金属性分析，发现[ Fe / H ] = - 0.09 ± 0.16 $$ left[mathrm{Fe}/mathrm{H}right]=-0.09pm 0.16 $$ 和 [ Fe / H ] = - 0.20 ± 0.20 $$ left[mathrm{Fe}/mathrm{H}right]=-0.20pm 0.20 $dex 分别为 Rup-1 和 Rup-171.年龄和距离是基于UBV和Gaia数据分析得出的；根据等时线拟合，估计Rup-1的年龄为t = 580 ± 60 $ t=580pm 60 $ Myr，d = 1469 ± 57 $ d=1469pm 57 $ pc；Rup-171的年龄为t = 2700 ± 200 $ t=2700pm 200 $ Myr，d = 1509 ± 69 $ d=1509pm 69 $ pc。Rup-1的现今质量函数斜率估计为1.26 ± 0.32 $$ 1.26pm 0.32 $$，Rup-171为1.53 ± 1.49 $$ 1.53pm 1.49 $$。银河轨道积分分析表明，这两个星团可能都是在太阳圈外形成的。

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引用次数: 0

Cover Picture: Astron. Nachr. 7/2024 封面图片：Astron.Nachr.7/2024

IF 1.1 4区物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS

Astronomische Nachrichten

Pub Date : 2024-08-20 DOI: 10.1002/asna.20249015

Klaus G. Strassmeier, Ilya Ilyin, Manfred Woche, Frank Dionies, Michael Weber, Arto Järvinen, Carsten Denker, Ekaterina Dineva, Meetu Verma, Thomas Granzer, Wilbert Bittner, Svend-Marian Bauer, Jens Paschke, Hakan Önel

First-light spectra of the Sun as a star taken by SDI-POL, the Solar Disk Integration POLarimeter feeding the PEPSI night-time spectrograph at the LBT. The top panel shows the full wavelength range (383 - 907 nm) covered by SDI-POL. The color of the Stokes I spectra indicates the individual cross dispersers; dark blue (=CD 1) to dark red (=CD 6). The line at the bottom represents the normalized Stokes V Q & U signal on the same intensity scale as Stokes I. The bottom panel is a zoom into the spectral region around the sodium D lines. The top spectrum is again Stokes I (plotted are dots per CCD pixel connected by a line), the bottom spectra are Stokes V Q U shifted by -0.10 in intensity and expanded by a factor 200 in scale with respect to Stokes I. The I Q U spectrum was taken on UT May 20, 2022, the V-spectrum on UT June 22, 2023. The first-light application detects a clear Stokes V/I profile indicative of a tiny but significant solar disk-averaged line-of-sight net magnetic field of +0.37±0.02 Gauß on Oct. 13, 2023, as reported in the article by Strassmeier et al., this issue, e240033.

由 SDI-POL 拍摄的太阳作为恒星的第一光光谱，SDI-POL 是太阳盘面积分光度计，为 LBT 的 PEPSI 夜用光谱仪提供能量。上图显示了 SDI-POL 覆盖的整个波长范围（383 - 907 nm）。斯托克斯 I光谱的颜色表示各个交叉色散器；从深蓝色（=CD 1）到深红色（=CD 6）。底图是钠 D 线附近光谱区域的放大图。上面的光谱也是斯托克斯 I 波段（每个 CCD 像素上的点用一条线连接），下面的光谱是斯托克斯 V Q U 波段，强度偏移了-0.10，相对于斯托克斯 I 波段的比例扩大了 200 倍。I Q U 波段拍摄于 2022 年 5 月 20 日UT，V 波段拍摄于 2023 年 6 月 22 日UT。第一光应用探测到了清晰的斯托克斯 V/I 曲线，表明 2023 年 10 月 13 日太阳盘平均视线净磁场为 +0.37±0.02 Gauß，虽然微小，但意义重大，正如 Strassmeier 等人的文章（本期，e240033）所报道的那样。

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