bluuebunny/crossref_metadata_2025_split huggingface dataset:
MOTIVASI TERHADAP KINERJA KARYAWAN DENGAN DISIPLIN KERJA DAN EMPLOYEE ENGAGEMENT SEBAGAI VARIABEL MEDIASI DI BAGIAN KEUANGAN RS X
Authors: Hania Rabia Nur , Bernardus Denny 
Published: October 2021

Human resources is a device that is used by every organization or company to achieve it’s goal. The success of an organization or company is the result of maximum performance of on employee in that company, the company will not run or succed if the employee cannot work well, therefore the development og good human resource must be created by a company. The purpose of this research is to evaluate the influence of motivation on employee performance, motivation on work discipline, motivation on employee engagement, work discipline on employee performance, employee engagement on employee performance, motivation on employee performance is mediated by work discipline, and motivation on employee performance is mediated by employee engagement. This research was conducted in the financial department of RS X with the total population and sample of 49 people. The method that is used in this research is quantitative by using primary and secondary data types. Data collection technique is by using questionnaire. Data analysis methods use SEM-PLS. Outcome of the research shows that motivational variable have positive, significant effect towards employees’ performance, work discipline and employee engagement. Work discipline variable mediated connect to employes’ performance. Work discipline variable mediates connection between motivational and employees’ performance, cause a positive and significant effect. Likewise with employee engagement variable mediate the relationship between motivation on employee performance and influence positive and significant.
Keywords : Employee Engagement,Employee Performance,Motivation, Work Discipline
PENGARUH PASSION DAN LINGKUNGAN KERJA NON FISIK TERHADAP KINERJA MAHASISWA DALAM MENJALANKAN BISNIS
Authors: Halim Stefanus Alvian 
Published: October 2021

Entrepreneurship memiliki peran yang penting bagi perekonomian negara, sedangkan jumlah entrepreneur Indonesia masih tertinggal dari standar negara maju. Oleh karena itu pemerintah memberikan dorongan kepada universitas untuk memberikan pengajaran entrepreneur sehingga nantinya lulusan universitas diharapkan mampu mendirikan bisnis serta menciptakan lapangan pekerjaan. Untuk dapat mendirikan bisnis yang memiliki kinerja baik, terdapat beberapa faktor yang mempengaruhinya diantaranya yaitu passion dan juga lingungan kerja non fisik dan terdapat pengaruh lain seperti budaya hingga manajemen waktu. Penelitian yang dilakukan ini bertujuan untuk menganalisis pengaruh passion dan lingkungan kerja non fisik terhadap kinerja mahasiswa dalam menjalankan bisnis. Metode yang digunakan untuk mengumpulkan data menggunakan kuesioner yang disebar secara online melalui googleform kepada 155 mahasiswa Universitas Ciputra angkatan 2016 yang sedang mengikuti mata kuliah IRBP dan memiliki start-up business. Teknik Pengambilan sampel dilakukan dengan menggunakan purposive sampling dengan penentuan jumlah minimal menggunakan rumus slovin. Penelitian ini merupakan penelitian kuantitatif dengan pengolahan data menggunakan regresi linear berganda melalui program SPSS. Hasilnya menunjukan bahwa passion dan juga lingkungan kerja non fisik, baik secara parsial maupun secara simultan berpengaruh positif dan signifikan terhadap kinerja mahasiswa Universitas Ciputra dalam menjalankan bisnis. Dengan hasil ini diharapkan mahasiswa mampu mendirikan bisnis sesuai dengan passion yang dimiliki serta menciptakan lingkungan kerja non fisik yang baik bagi perusahaan yang dijalankan agar perusahaan dan juga stakeholder mampu memiliki kinerja yang baik.

Kata kunci:passion, lingkungan kerja non fisik, kinerja, entrepreneur
Evidence of a Tidal-disruption Event in GSN 069 from the Abnormal Carbon and Nitrogen Abundance Ratio
Authors: Sheng Zhenfeng , Wang Tinggui , Ferland Gary , Shu Xinwen , Yang Chenwei , Jiang Ning , Chen Yang 
Published: October 2021

Abstract
GSN 069 is an ultra-soft X-ray active galactic nucleus that previously exhibited a huge X-ray outburst and a subsequent long-term decay. It has recently presented X-ray quasi-periodic eruptions (QPEs). We report the detection of strong nitrogen lines but weak or undetectable carbon lines in its far-ultraviolet spectrum. With a detailed photoionization model, we use the C iv/N iv] ratio and other ratios between nitrogen lines to constrain the [C/N] abundance of GSN 069 to be from −3.33 to −1.91. We argue that a partially disrupted red giant star can naturally explain the abnormal C/N abundance in the UV spectrum, while the surviving core orbiting the black hole might produce the QPEs.
The TESS View of LOFAR Radio-emitting Stars
Authors: Pope Benjamin J. S. , Callingham Joseph R. , Feinstein Adina D. , Günther Maximilian N. , Vedantham Harish K. , Ansdell Megan , Shimwell Timothy W. 
Published: October 2021

Abstract
The recent detection of the M dwarf GJ 1151 at 144 MHz low radio frequencies using LOFAR has been interpreted as evidence of an exoplanet magnetically interacting with its host star. This would be the first exoplanet detected around a main-sequence star by a radio telescope. Radial velocity confirmation of such a planet has proven inconclusive and it remains possible that the radio emission could be generated by a stellar coronal process. Using data from TESS, we shed light on this question by probing the stellar activity and flares of GJ 1151 as well as 14 other M dwarfs detected by LOFAR. GJ 1151 and three other star–planet interaction candidates are found to be inactive, with no rotational modulation and few, if any, flares. The remainder of the LOFAR-detected M dwarfs flare frequently. We consider it unlikely that stellar activity is responsible for the bright, circularly polarized emission from GJ 1151 and its three analogs and support the star–planet magnetic interaction interpretation.
Morphological Transition of the Compact Radio Lobe in 3C 84 via the Strong Jet–Cloud Collision
Authors: Kino Motoki , Niinuma Kotaro , Kawakatu Nozomu , Nagai Hiroshi , Giovannini Gabriele , Orienti Monica , Wajima Kiyoaki , D’Ammando Filippo , Hada Kazuhiro , Giroletti Marcello , Gurwell Mark 
Published: October 2021

Abstract
We report multiepoch very long baseline interferometric observations of the compact radio lobe in the radio galaxy 3C 84 (NGC 1275) during 2016–2020. The image sequence of 3C 84 reveals that the hotspot in the radio lobe showed the 1 year long frustration in 2017 within a compact region of about 0.07 pc, suggesting a strong collision between the jet and a compact dense cloud with an estimated average density of about (4–6) × 105 cm−3. Although the hotspot and the radio lobe began to move south again after its breakout, the radio lobe showed a morphological transition from an FR II- to FR I-class radio lobe and its radio flux became fainter. This is the first detection of the dynamical feedback from the cloud to the jet where the cloud located on the jet axis significantly interferes with the jet propagation and evolution at the central 1 pc region in the active galactic nucleus.
TOI-3362b: A Proto Hot Jupiter Undergoing High-eccentricity Tidal Migration
Authors: Dong Jiayin , Huang Chelsea X. , Zhou George , Dawson Rebekah I. , Rodriguez Joseph E. , Eastman Jason D. , Collins Karen A. , Quinn Samuel N. , Shporer Avi , Triaud Amaury H. M. J. , Wang Songhu , Beatty Thomas , Jackson Jonathon M. , Collins Kevin I. , Abe Lyu , Suarez Olga , Crouzet Nicolas , Mékarnia Djamel , Dransfield Georgina , Jensen Eric L. N. , Stockdale Chris , Barkaoui Khalid , Heitzmann Alexis , Wright Duncan J. , Addison Brett C. , Wittenmyer Robert A. , Okumura Jack , Bowler Brendan P. , Horner Jonathan , Kane Stephen R. , Kielkopf John , Liu Huigen , Plavchan Peter , Mengel Matthew W. , Ricker George R. , Vanderspek Roland , Latham David W. , Seager S. , Winn Joshua N. , Jenkins Jon M. , Christiansen Jessie L. , Paegert Martin 
Published: October 2021

Abstract
High-eccentricity tidal migration is a possible way for giant planets to be placed in short-period orbits. If this happens often, one would expect to catch proto hot Jupiters on highly elliptical orbits undergoing high-eccentricity tidal migration. As of yet, few such systems have been discovered. Here, we introduce TOI-3362b (TIC-464300749b), an 18.1 day, 5 M
Jup planet orbiting a main-sequence F-type star that is likely undergoing high-eccentricity tidal migration. The orbital eccentricity is 0.815

−
0.032

+
0.023

. With a semimajor axis of 0.153

−
0.003

+
0.002

au, the planet’s orbit is expected to shrink to a final orbital radius of 0.051

−
0.006

+
0.008

au after complete tidal circularization. Several mechanisms could explain the extreme value of the planet’s eccentricity, such as planet–planet scattering and secular interactions. Such hypotheses can be tested with follow-up observations of the system, e.g., measuring the stellar obliquity and searching for companions in the system with precise, long-term radial-velocity observations. The variation in the planet’s equilibrium temperature as it orbits the host star and the tidal heating at periapse make this planet an intriguing target for atmospheric modeling and observation. Because the planet’s orbital period of 18.1 days is near the limit of TESS’s period sensitivity, even a few such discoveries suggest that proto hot Jupiters may be quite common.
Comparison of Anomalous and Galactic Cosmic-Ray Oxygen at 1 au during 1997–2020
Authors: Fu Shuai , Zhao Lingling , Zhang Xiaoping , Luo Pengwei , Li Yong 
Published: October 2021

Abstract
Using quiet-time measurements of element oxygen within the energy range 7.3–237.9 MeV nuc−1 from the ACE spacecraft at 1 au, we compare the energy spectra and intensities of anomalous and Galactic cosmic rays (ACRs and GCRs, respectively) during 1997–2020. Our analysis shows that the transition from the ACR-dominated spectrum to the GCR-dominated spectrum occurs at energies ∼15 to ∼35 MeV nuc−1, and the transition energy E

t
is found to be well anticorrelated with varying solar activity. This is the first study of ACR–GCR transition energy dependence on the solar cycle variation. At energies below E

t
, the index of the power-law ACR-dominated spectrum (γ
1) ranges from −2.0 to −0.5, whereas the GCR-dominated spectrum has a power-law index (γ
2) changing from 0.3 to 0.8 at energies ranging from E

t
to 237.9 MeV nuc−1. Both γ
1 and γ
2 are positively correlated with solar activity. In addition, during the solar cycle 24/25 minimum period, the peak GCR intensity observed by ACE spacecraft is about 8% above its 2009 value, setting a new record since the space age, while the peak ACR intensity is almost similar to that of the previous two solar cycles with the same pattern of solar magnetic polarity, indicating a different modulation mechanism between ACRs and GCRs.
The Effects of Dark Matter and Baryonic Physics on the Milky Way Subhalo Population in the Presence of the Large Magellanic Cloud
Authors: Nadler Ethan O. , Banerjee Arka , Adhikari Susmita , Mao Yao-Yuan , Wechsler Risa H. 
Published: October 2021

Abstract
Given recent developments in our understanding of the Large Magellanic Cloud's (LMC) impact on the Milky Way's (MW) dark matter subhalo population, we compare the signatures of dark matter and baryonic physics on subhalos in MW systems with realistic LMC analogs. In particular, we study the effects of self-interacting dark matter (SIDM), warm dark matter (WDM), and the Galactic disk on the peak maximum circular velocity (V
peak) function, radial distribution, and spatial distribution of MW and LMC-associated subhalos using cosmological dark matter-only zoom-in simulations of MW+LMC systems. For a fixed abundance of subhalos expected to host dwarf galaxies (V
peak ≳ 20 km s−1), SIDM and WDM can produce a similar mass-dependent suppression of the subhalo V
peak function, while disk disruption is mass independent. Subhalos in the inner regions of the MW are preferentially disrupted by both self-interactions and the disk, while suppression in WDM is radially independent. The relative abundance of LMC-associated subhalos is not strongly affected by disk disruption or WDM, but is significantly suppressed in SIDM due to self-interactions with the LMC at early times and with the MW during LMC infall at late times, erasing spatial anisotropy in the MW subhalo population. These results provide avenues to distinguish dark matter and baryonic physics by combining properties of the MW and LMC subhalo populations probed by upcoming observations of satellite galaxies and stellar streams.
Energy and Waiting Time Distributions of FRB 121102 Observed by FAST
Authors: Zhang G. Q. , Wang P. , Wu Q. , Wang F. Y. , Li D. , Dai Z. G. , Zhang B. 
Published: October 2021

Abstract
The energy and waiting time distributions are important properties for understanding the physical mechanism of repeating fast radio bursts (FRBs). Recently, the Five-hundred-meter Aperture Spherical radio Telescope (FAST; Nan et al. 2011; Li et al. 2018) detected the largest burst sample of FRB 121102, containing 1652 bursts Li et al. (2021a) We use this sample to investigate the energy and waiting time distributions. The energy count distribution dN/dE at the high-energy range (>1038 erg) can be fitted with a single power-law function with an index of

−

1.86

−
0.02

+
0.02

, while the distribution at the low-energy range deviates from the power-law function. An interesting result of Li et al. (2021a) is that there is an apparent temporal gap between early bursts (occurring before MJD 58740) and late bursts (occurring after MJD 58740). We find that the energy distributions of high-energy bursts at different epochs are inconsistent. The power-law index is

−

1.70

−
0.03

+
0.03

for early bursts and

−

2.60

−
0.14

+
0.15

for late bursts. For bursts observed in a single day, a linear repetition pattern is found. We use the Weibull function to fit the distribution of waiting time of consecutive bursts. The shape parameter

k
=

0.72

−
0.01

+
0.01

and the event rate

r
=

736.43

−
28.90

+
26.55

day−1 are derived. If the waiting times with δ

t
< 28 s are excluded, the burst behavior can be described by a Poisson process. The best-fitting values of k are slightly different for low-energy (E < 1.58 × 1038 erg) and high-energy (E > 1.58 × 1038 erg) bursts.
Some First Stars Were Red: Detecting Signatures of Massive Population III Formation through Long-term Stochastic Color Variations
Authors: Woods Tyrone E. , Willott Chris J. , Regan John A. , Wise John H. , Downes Turlough P. , Norman Michael L. , O’Shea Brian W. 
Published: October 2021

Abstract
Identifying stars formed in pristine environments (Population III) within the first billion years is vital to uncovering the earliest growth and chemical evolution of galaxies. Population III galaxies, however, are typically expected to be too faint and too few in number to be detectable by forthcoming instruments without extremely long integration times and/or extreme lensing. In an environment, however, where star formation is suppressed until a halo crosses the atomic-cooling limit (e.g., by a modest Lyman–Werner flux, high baryonic streaming velocities, and/or dynamical heating effects), primordial halos can form substantially more numerous and more massive stars. Some of these stars will in turn be accreting more rapidly than they can thermally relax at any given time. Using high-resolution cosmological zoom-in simulations of massive star formation in high-z halos, we find that such rapidly accreting stars produce prominent spectral features that would be detectable by the James Webb Space Telescope. The rapid-accretion episodes within the halo lead to stochastic reprocessing of 0%–20% of the total stellar emission into the rest-frame optical over long timescales, a unique signature which may allow deep observations to identify such objects out to z ∼ 10–13 using mid- and wide-band NIRCam colors alone.
Asymmetric H i 21 cm Lines of Fast Radio Burst Hosts: Connection with Galaxy Interaction
Authors: Michałowski Michał J. 
Published: October 2021

Abstract
Fast radio bursts (FRBs) are enigmatic transients with very short radio emission. Their nature is still widely debated. I provide the first analysis of atomic gas properties of a small sample of FRB hosts to constrain their nature. H i observations exist for NGC 3252, the host of FRB 181030A, M81, the host of FRB 200120E, and the Milky Way, the host of FRB 200428. I report three observables: (i) all three FRB hosts are interacting galaxies; (ii) the H i spectra of both FRB hosts with such data available are highly asymmetric, several standard deviations above the general population of galaxies; (iii) two FRB hosts have normal atomic gas properties and one is strongly deficient in atomic gas. This indicates that nearby and repeating FRBs are connected with a recent enhancement of star formation due to interaction. This supports fast FRB channels, for example, a massive star with a short delay time so that interaction signatures giving rise to the birth of the progenitor are still visible. Long gamma-ray burst (GRB) and broad-lined type Ic supernova (SN) hosts exhibit much more symmetric spectra, even though they were claimed to experience gas inflow from the intergalactic medium. The difference can be explained by the interactions experienced by FRB hosts being more disruptive than these gas inflows, or by the mass effect, with GRB/SN hosts at lower masses having less organized gas motions, so with H i lines closer to a symmetrical Gaussian. This also suggests that the emission mechanisms of FRBs and GRBs are different.
On the Large Apparent Black Hole Spin-orbit Misalignment Angle in GW200115
Authors: Zhu Xing-Jiang 
Published: October 2021

Abstract
GW200115 is one of the first two confidently detected gravitational-wave events of neutron star–black hole mergers. An interesting property of this merger is that the black hole, if spinning rapidly, has its spin axis negatively aligned (with a misalignment angle >90°) with the binary orbital angular momentum vector. Although such a large spin–orbit misalignment angle naturally points toward a dynamical origin, the measured neutron star–black hole merger rate exceeds theoretical predictions of the dynamical formation channel. In the canonical isolated binary formation scenario, the immediate progenitor of GW200115 is likely to be a binary consisting of a black hole and a helium star, with the latter forming a neutron star during a supernova explosion. Since the black hole is generally expected to spin along the pre-supernova binary orbital angular momentum axis, a large neutron star natal kick is required to produce the observed misalignment angle. Using simple kinematic arguments, we find that a misalignment angle >90° in GW200115-like systems implies a kick velocity ∼600 km s−1 and a kick direction within ≈30° of the pre-supernova orbital plane. We discuss different interpretations of the large apparent black hole spin–orbit misalignment angle, including a nonspinning black hole.
Long GMC Lifetimes: Using the Method and Data of Meidt et al. (2015) with a Correction
Authors: Koda Jin 
Published: October 2021

Abstract
Meidt et al. derived short lifetimes of 20–30 Myr for giant molecular clouds (GMCs) in M51. Their novel approach utilizes a decline of the GMC population during their inter-arm passage from one spiral arm to the next. Using the inter-arm travel time t
travel as a fiducial clock, they converted the decline rate to GMC lifetimes. They implicitly adopted zero as the pattern speed of the spiral arms, resulting in a very short t
travel. However, it is well established that the spiral arm pattern in M51 is rotating, and that t
travel should be measured with respect to the rotating spiral pattern. Here we use the same method and data of Meidt et al. and re-evaluate GMC lifetimes by accounting for the pattern speed given by Meidt et al. This correction gives a longer t
travel, and consequently longer GMC lifetimes of 60–500 Myr.
K-band Luminosity Functions of IllustrisTNG300-1 Galaxies
Authors: Brainerd Tereasa G. 
Published: October 2021

Abstract
This Research Note summarizes preliminary results, presented at the 238th AAS meeting, for the K-band luminosity functions (LFs) of IllustrisTNG300-1 galaxies. For M

K
≥ −22, the simulation reproduces both the shape and amplitude of the LF for observed field galaxies. However, it significantly overproduces field galaxies with M

K
< −22. For M

K
≤ −22, the simulation reproduces the shape of the LF for observed cluster galaxies, however at fainter magnitudes the LF falls below a simple extrapolation of recent observations. For M

K
≤ −22, the shapes of the LFs for red cluster galaxies and blue cluster galaxies agree reasonably well with observations, but neither is well-fitted by a Schechter function at fainter magnitudes. In addition, the faint-end slope of the LF in the inner regions of the clusters is significantly flatter than it is in the outer regions.
Evolution of the Gas Density in a Simulated Star-forming Cloud with Stellar Feedback
Authors: Lue Amanda , Guszejnov Dávid , Offner Stella S. R. , Grudić Michael Y. 
Published: October 2021

Abstract
Star formation involves gravity, turbulence, magnetic fields, and feedback from new stars through jets, radiation and winds. The evolution of the density probability distribution function (ρ-PDF) is directly related to the star formation rate (SFR), forming the basis of several star formation models. We utilize two runs from the STARFORGE simulation suite that follow the evolution of molecular clouds, while resolving individual stars and including all gas and feedback physics. The two runs have different initial conditions, one is a periodic box with driven turbulence (Box), while the other is an isolated cloud without turbulent driving (Sphere). We find that the ρ-PDF for both runs is initially well-fit by a log-normal (LN) plus a power-law (PL) function. However, as the SFR peaks, the PDF for the Sphere run becomes well-fit by just a wide LN. Conversely, the Box run PDF remains well-fit by a LN+PL function for the entirety of the run.
VeSPA: The SuperWASP Variable Star Photometry Archive
Authors: McMaster Adam , Norton Andrew J. , Dickinson Hugh J. , Thiemann Heidi B. , Kolb Ulrich C. 
Published: October 2021

Abstract
We present the first results from the SuperWASP Variable Stars (SVS) citizen science project. The photometry archive of the Wide Angle Search for Planets has previously been searched for periodic variations and the results of this search formed the basis of the SVS project on the Zooniverse. The SVS project asks volunteers to visually inspect light curve plots and categorize each one according to a broad classification scheme. Results from the first two years of SVS have now been published online as the SuperWASP Variable Star Photometry Archive (VeSPA). The archive can be browsed online, downloaded in full, or queried, filtered, and sorted to export a refined set of results. An interactive light curve viewer also allows any light curve to be folded at a user-defined period. Analysis of citizen science results and development of VeSPA features are both ongoing. Updated results will be published every six months.
Discovery of a Uniquely Cool and Compact Source at 28 pc from the Sun
Authors: Apps Kevin , Smart R. L. , Silvotti Roberto 
Published: October 2021

Abstract
We present the discovery of what appears to be both a uniquely cool and old white dwarf (WD) within 30 pc of the Sun. DES J214756.46-403529.3 is detected in four separate surveys, 50° away from the Galactic Plane. The combination of its very low luminosity and spectral energy distribution suggests an object unlike any other astrophysical body currently known. Among 8000 of the nearest single objects in the immediate solar neighborhood, it appears completely isolated in multiple color–magnitude diagrams. The data seem compatible with an extremely old and cool WD with a helium dominated atmosphere and a mass around 0.7–0.8 M
⊙ but spectroscopic follow-up is required to confirm its nature.