TY - JOUR A1 - Gruner, David A1 - Hainich, Rainer A1 - Sander, Andreas Alexander Christoph A1 - Shenar, Tomer A1 - Todt, Helge Tobias A1 - Oskinova, Lidia M. A1 - Ramachandran, Varsha A1 - Ayres, T. A1 - Hamann, Wolf-Rainer T1 - The extreme O-type spectroscopic binary HD 93129A A quantitative, multiwavelength analysis JF - Astronomy and astrophysics : an international weekly journal N2 - Context. HD 93129A was classified as the earliest O-type star in the Galaxy (O2 If*) and is considered as the prototype of its spectral class. However, interferometry shows that this object is a binary system, while recent observations even suggest a triple configuration. None of the previous spectral analyses of this object accounted for its multiplicity. With new high-resolution UV and optical spectra, we have the possibility to reanalyze this key object, taking its binary nature into account for the first time. Aims. We aim to derive the fundamental parameters and the evolutionary status of HD 93129A, identifying the contributions of both components to the composite spectrum Results. Despite the similar spectral types of the two components, we are able to find signatures from each of the components in the combined spectrum, which allows us to estimate the parameters of both stars. We derive log(L/L-circle dot) = 6.15, T-eff = 52 kK, and log (M)over dot = -4.7[M-circle dot yr(-1)] for the primary Aa, and log(L/L-circle dot) = 5.58, T-eff = 45 kK, and log (M)over dot = -5.8 [M(circle dot)yr(-1)] for the secondary Ab. Conclusions. Even when accounting for the binary nature, the primary of HD 93129A is found to be one of the hottest and most luminous O stars in our Galaxy. Based on the theoretical decomposition of the spectra, we assign spectral types O2 If* and O3 III(f*) to components Aa and Ab, respectively. While we achieve a good fit for a wide spectral range, specific spectral features are not fully reproduced. The data are not sufficient to identify contributions from a hypothetical third component in the system. KW - stars: individual: HD 93129A KW - stars: atmospheres KW - stars: fundamental parameters KW - stars: early-typeP Y1 - 2018 U6 - https://doi.org/10.1051/0004-6361/201833178 SN - 1432-0746 VL - 621 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Robrade, Jan A1 - Oskinova, Lidia M. A1 - Schmitt, J. H. M. M. A1 - Leto, Paolo A1 - Trigilio, C. T1 - Outstanding X-ray emission from the stellar radio pulsar CU Virginis JF - Astronomy and astrophysics : an international weekly journal N2 - Context. Among the intermediate-mass magnetic chemically peculiar (MCP) stars, CU Vir is one of the most intriguing objects. Its 100% circularly polarized beams of radio emission sweep the Earth as the star rotates, thereby making this strongly magnetic star the prototype of a class of nondegenerate stellar radio pulsars. While CU Vir is well studied in radio, its high-energy properties are not known. Yet, X-ray emission is expected from stellar magnetospheres and confined stellar winds. Aims. Using X-ray data we aim to test CU Vir for intrinsic X-ray emission and investigate mechanisms responsible for its generation. Methods. We present X-ray observations performed with XMM-Newton and Chandra and study obtained X-ray images, light curves, and spectra. Basic X-ray properties are derived from spectral modelling and are compared with model predictions. In this context we investigate potential thermal and nonthermal X-ray emission scenarios. Results. We detect an X-ray source at the position of CU Vir. With LX approximate to 3 x 10(28) erg s(-1) it is moderately X-ray bright, but the spectrum is extremely hard compared to other Ap stars. Spectral modelling requires multi-component models with predominant hot plasma at temperatures of about T-X = 25MK or, alternatively, a nonthermal spectral component. Both types of model provide a virtually equivalent description of the X-ray spectra. The Chandra observation was performed six years later than those by XMM-Newton, yet the source has similar X-ray flux and spectrum, suggesting a steady and persistent X-ray emission. This is further confirmed by the X-ray light curves that show only mild X-ray variability. Conclusions. CU Vir is also an exceptional star at X-ray energies. To explain its full X-ray properties, a generating mechanism beyond standard explanations, like the presence of a low-mass companion or magnetically confined wind-shocks, is required. Magnetospheric activity might be present or, as proposed for fast-rotating strongly magnetic Bp stars, the X-ray emission of CU Vir is predominantly auroral in nature. KW - individual: CU Vir KW - stars: activity KW - stars: chemically peculiar KW - stars: magnetic field KW - X-rays: stars Y1 - 2018 U6 - https://doi.org/10.1051/0004-6361/201833492 SN - 1432-0746 VL - 619 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Leto, Paolo A1 - Trigilio, C. A1 - Oskinova, Lidia M. A1 - Ignace, R. A1 - Buemi, C. S. A1 - Umana, G. A1 - Ingallinera, A. A1 - Leone, Francesco A1 - Phillips, N. M. A1 - Agliozzo, Claudia A1 - Todt, Helge Tobias A1 - Cerrigone, L. T1 - A combined multiwavelength VLA/ALMA/Chandra study unveils the complex magnetosphere of the B-type star HR5907 JF - Monthly notices of the Royal Astronomical Society N2 - We present new radio/millimeter measurements of the hot magnetic star HR5907 obtained with the VLA and ALMA interferometers. We find that HR5907 is the most radio luminous early type star in the cm-mm band among those presently known. Its multi-wavelength radio light curves are strongly variable with an amplitude that increases with radio frequency. The radio emission can be explained by the populations of the non-thermal electrons accelerated in the current sheets on the outer border of the magnetosphere of this fast-rotating magnetic star. We classify HR5907 as another member of the growing class of strongly magnetic fast-rotating hot stars where the gyro-synchrotron emission mechanism efficiently operates in their magnetospheres. The new radio observations of HR5907 are combined with archival X-ray data to study the physical condition of its magnetosphere. The X-ray spectra of HR5907 show tentative evidence for the presence of non-thermal spectral component. We suggest that non-thermal X-rays originate a stellar X-ray aurora due to streams of non-thermal electrons impacting on the stellar surface. Taking advantage of the relation between the spectral indices of the X-ray power-law spectrum and the non-thermal electron energy distributions, we perform 3-D modelling of the radio emission for HR5907. The wavelength-dependent radio light curves probe magnetospheric layers at different heights above the stellar surface. A detailed comparison between simulated and observed radio light curves leads us to conclude that the stellar magnetic field of HR 5907 is likely non-dipolar, providing further indirect evidence of the complex magnetic field topology of HR5907. KW - stars: chemically peculiar KW - stars: early-type KW - stars: individual: HR 5907 KW - stars: magnetic field KW - radio continuum: stars KW - X-rays: stars Y1 - 2018 U6 - https://doi.org/10.1093/mnras/sty244 SN - 0035-8711 SN - 1365-2966 VL - 476 IS - 1 SP - 562 EP - 579 PB - Oxford Univ. Press CY - Oxford ER - TY - JOUR A1 - Oskinova, Lidia M. A1 - Bulik, Tomasz A1 - Gomez-Moran, Ada Nebot T1 - Infrared outbursts as potential tracers of common-envelope events in high-mass X-ray binary formation JF - Astronomy and astrophysics : an international weekly journal N2 - Context. Classic massive binary evolutionary scenarios predict that a transitional common-envelope (CE) phase could be preceded as well as succeeded by the evolutionary stage when a binary consists of a compact object and a massive star, that is, a high-mass X-ray binary (HMXB). The observational manifestations of common envelope are poorly constrained. We speculate that its ejection might be observed in some cases as a transient event at mid-infrared (IR) wavelengths. Aims. We estimate the expected numbers of CE ejection events and HMXBs per star formation unit rate, and compare these theoretical estimates with observations. Methods. We compiled a list of 85 mid-IR transients of uncertain nature detected by the Spitzer Infrared Intensive Transients Survey and searched for their associations with X-ray, optical, and UV sources. Results. Confirming our theoretical estimates, we find that only one potential HMXB may be plausibly associated with an IR-transient and tentatively propose that X-ray source NGC4490-X40 could be a precursor to the SPIRITS 16az event. Among other interesting sources, we suggest that the supernova remnant candidate [BWL2012] 063 might be associated with SPIRITS 16ajc. We also find that two SPIRITS events are likely associated with novae, and seven have potential optical counterparts. Conclusions. The massive binary evolutionary scenarios that involve CE events do not contradict currently available observations of IR transients and HMXBs in star-forming galaxies. KW - X-rays: binaries KW - stars: massive KW - infrared: general KW - infrared: galaxies Y1 - 2018 U6 - https://doi.org/10.1051/0004-6361/201832925 SN - 0004-6361 SN - 1432-0746 VL - 613 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - González-Galán, Ana A1 - Oskinova, Lidia M. A1 - Popov, Sergei B. A1 - Haberl, F. A1 - Kühnel, M. A1 - Gallagher, John S. A1 - Schurch, Matthew A1 - Guerrero, Martín A. T1 - A multiwavelength study of SXP 1062, the long-period X-ray pulsar associated with a supernova remnant JF - Monthly notices of the Royal Astronomical Society N2 - SXP 1062 is a Be X-ray binary (BeXB) located in the Small Magellanic Cloud. It hosts a long-period X-ray pulsar and is likely associated with the supernova remnant MCSNR J0127−7332. In this work we present a multiwavelength view on SXP 1062 in different luminosity regimes. We consider monitoring campaigns in optical (OGLE survey) and X-ray (Swift telescope). During these campaigns a tight coincidence of X-ray and optical outbursts is observed. We interpret this as typical Type I outbursts as often detected in BeXBs at periastron passage of the neutron star (NS). To study different X-ray luminosity regimes in depth, during the source quiescence we observed it with XMM–Newton while Chandra observations followed an X-ray outburst. Nearly simultaneously with Chandra observations in X-rays, in optical the RSS/SALT telescope obtained spectra of SXP 1062. On the basis of our multiwavelength campaign we propose a simple scenario where the disc of the Be star is observed face-on, while the orbit of the NS is inclined with respect to the disc. According to the model of quasi-spherical settling accretion our estimation of the magnetic field of the pulsar in SXP 1062 does not require an extremely strong magnetic field at the present time. KW - stars: neutron KW - pulsars: individual: SXP 1062 KW - galaxies: individual: Small Magellanic Cloud KW - X-rays: binaries Y1 - 2017 U6 - https://doi.org/10.1093/mnras/stx3127 SN - 0035-8711 SN - 1365-2966 VL - 475 IS - 2 SP - 2809 EP - 2821 PB - Oxford University Press CY - Oxford ER - TY - JOUR A1 - Martinez-Chicharro, M. A1 - Torrejon, J. M. A1 - Oskinova, Lidia M. A1 - Furst, F. A1 - Postnov, K. A1 - Rodes-Roca, J. J. A1 - Hainich, Rainer A1 - Bodaghee, A. T1 - Evidence of Compton cooling during an X-ray flare supports a neutron star nature of the compact object in 4U1700-37 JF - Monthly notices of the Royal Astronomical Society N2 - Based on new Chandra X-ray telescope data, we present empirical evidence of plasma Compton cooling during a flare in the non-pulsating massive X-ray binary 4U1700-37. This behaviour might be explained by quasi-spherical accretion on to a slowly rotating magnetized neutron star (NS). In quiescence, the NS in 4U1700-37 is surrounded by a hot radiatively cooling shell. Its presence is supported by the detection of mHz quasi-periodic oscillations likely produced by its convection cells. The high plasma temperature and the relatively low X-ray luminosity observed during the quiescence, point to a small emitting area similar to 1 km, compatible with a hotspot on an NS surface. The sudden transition from a radiative to a significantly more efficient Compton cooling regime triggers an episode of enhanced accretion resulting in a flare. During the flare, the plasma temperature drops quickly. The predicted luminosity for such transitions, similar to 3 x 10(35) erg s(-1), is very close to the luminosity of 4U1700-37 during quiescence. The transition may be caused by the accretion of a clump in the stellar wind of the donor star. Thus, a magnetized NS nature of the compact object is strongly favoured. KW - stars: individual: 4U1700-37 KW - V*V884 Sco KW - X-rays: binaries Y1 - 2017 U6 - https://doi.org/10.1093/mnrasl/slx165 SN - 0035-8711 SN - 1365-2966 VL - 473 IS - 1 SP - L74 EP - L78 PB - Oxford Univ. Press CY - Oxford ER - TY - JOUR A1 - Torrejon, J. M. A1 - Reig, Pablo A1 - Fürst, F. A1 - Martinez-Chicharro, M. A1 - Postnov, K. A1 - Oskinova, Lidia M. T1 - NuSTAR rules out a cyclotron line in the accreting magnetar candidate 4U2206+54 JF - Monthly notices of the Royal Astronomical Society N2 - Based on our new NuSTAR X-ray telescope data, we rule out any cyclotron line up to 60 keV in the spectra of the high-mass X-ray binary 4U2206+54. In particular, we do not find any evidence of the previously claimed line around 30 keV, independently of the source flux, along the spin pulse. The spin period has increased significantly, since the last observation, up to 5750 +/- 10 s, confirming the rapid spin-down rate (nu)over dot = -1.8 x 10(-14) Hz s(-1). This behaviour might be explained by the presence of a strongly magnetized neutron star (B-s > several times 10(13) G) accreting from the slow wind of its main-sequence O9.5 companion. KW - Stars: individual: 4U2206+54, BD+53 2790 KW - X-rays: binaries Y1 - 2018 U6 - https://doi.org/10.1093/mnras/sty1628 SN - 0035-8711 SN - 1365-2966 VL - 479 IS - 3 SP - 3366 EP - 3372 PB - Oxford Univ. Press CY - Oxford ER - TY - JOUR A1 - Massa, Derck A1 - Oskinova, Lidia M. A1 - Prinja, Raman A1 - Ignace, Richard T1 - Coordinated UV and X-Ray Spectroscopic Observations of the O-type Giant xi Per BT - the Connection between X-Rays and Large-scale Wind Structure JF - The astrophysical journal : an international review of spectroscopy and astronomical physics N2 - We present new, contemporaneous Hubble Space Telescope STIS and XMM-Newton observations of the O7. III(n) ((f)) star xi Per. We supplement the new data with archival IUE spectra, to analyze the variability of the wind lines and X-ray flux of xi Per. The variable wind of this star is known to have a 2.086-day periodicity. We use a simple, heuristic spot model that fits the low-velocity (near-surface) IUE wind line variability very well, to demonstrate that the low-velocity absorption in the new STIS spectra of N IV lambda 1718 and Si IV lambda 1402 vary with the same 2.086-day period. It is remarkable that the period and amplitude of the STIS data agree with those of the IUE spectra obtained 22 yr earlier. We also show that the time variability of the new XMM-Newton fluxes is also consistent with the 2.086-day period. Thus, our new, multiwavelength coordinated observations demonstrate that the mechanism that causes the UV wind line variability is also responsible for a significant fraction of the X-rays in single O stars. The sequence of events for the multiwavelength light-curve minima is Si IV lambda 1402, N IV lambda 1718, and X-ray flux, each separated by a phase of about 0.06 relative to the 2.086-day period. Analysis of the X-ray fluxes shows that they become softer as they weaken. This is contrary to expectations if the variability is caused by periodic excess absorption. Furthermore, the high-resolution X-ray spectra suggest that the individual emission lines at maximum are more strongly blueshifted. If we interpret the low-velocity wind line light curves in terms of our model, it implies that there are two bright regions, i.e., regions with less absorption, separated by 180 degrees, on the surface of the star. We note that the presence and persistence of two spots separated by 180 degrees suggest that a weak dipole magnetic field is responsible for the variability of the UV wind line absorption and X-ray flux in xi Per. KW - stars: activity KW - stars: early-type KW - stars: winds, outflows KW - ultraviolet: stars KW - X-rays: stars Y1 - 2019 U6 - https://doi.org/10.3847/1538-4357/ab0283 SN - 0004-637X SN - 1538-4357 VL - 873 IS - 1 PB - IOP Publ. Ltd. CY - Bristol ER - TY - JOUR A1 - Oskinova, Lidia M. A1 - Feldmeier, Achim A1 - Hamann, Wolf-Rainer T1 - High-resolution X-ray spectroscopy of bright O-type stars JF - Monthly notices of the Royal Astronomical Society N2 - Archival X-ray spectra of the four prominent single, non-magnetic O stars zeta Pup, zeta Ori, xi Per and zeta Oph, obtained in high resolution with Chandra HETGS/MEG have been studied. The resolved X-ray emission line profiles provide information about the shocked, hot gas which emits the X-radiation, and about the bulk of comparably cool stellar wind material which partly absorbs this radiation. In this paper, we synthesize X-ray line profiles with a model of a clumpy stellar wind. We find that the geometrical shape of the wind inhomogeneities is important: better agreement with the observations can be achieved with radially compressed clumps than with spherical clumps. The parameters of the model, i.e. chemical abundances, stellar radius, mass-loss rate and terminal wind velocity, are taken from existing analyses of UV and optical spectra of the programme stars. On this basis, we also calculate the continuum-absorption coefficient of the cool-wind material, using the Potsdam Wolf-Rayet (POWR) model atmosphere code. The radial location of X-ray emitting gas is restricted from analysing the FIR line ratios of helium-like ions. The only remaining free parameter of our model is the typical distance between the clumps; here, we assume that at any point in the wind there is one clump passing by per one dynamical time-scale of the wind. The total emission in a model line is scaled to the observation. There is a good agreement between synthetic and observed line profiles. We conclude that the X-ray emission line profiles in O stars can be explained by hot plasma embedded in a cool wind which is highly clumped in the form of radially compressed shell fragments. KW - stars : individual : zeta Pup KW - stars : individual : zeta Ori KW - stars : individual : xi Per KW - stars : individual : zeta Oph KW - X-rays : stars Y1 - 2006 U6 - https://doi.org/10.1111/j.1365-2966.2006.10858.x SN - 0035-8711 VL - 372 SP - 313 EP - 326 PB - Oxford University Press CY - Oxford ER - TY - GEN A1 - Kubatova, Brankica A1 - Hamann, Wolf-Rainer A1 - Kubat, Jiri A1 - Oskinova, Lidia M. T1 - 3D Monte Carlo Radiative Transfer in Inhomogeneous Massive Star Winds BT - Application to Resonance Line Formation T2 - Radiative signatures from the cosmos N2 - Already for decades it has been known that the winds of massive stars are inhomogeneous (i.e. clumped). To properly model observed spectra of massive star winds it is necessary to incorporate the 3-D nature of clumping into radiative transfer calculations. In this paper we present our full 3-D Monte Carlo radiative transfer code for inhomogeneous expanding stellar winds. We use a set of parameters to describe dense as well as the rarefied wind components. At the same time, we account for non-monotonic velocity fields. We show how the 3-D density and velocity wind inhomogeneities strongly affect the resonance line formation. We also show how wind clumping can solve the discrepancy between P v and H alpha mass-loss rate diagnostics. Y1 - 2019 SN - 978-1-58381-925-8 SN - 1050-3390 VL - 519 SP - 209 EP - 212 PB - Astronomical soc pacific CY - San Fransisco ER - TY - JOUR A1 - Hainich, Rainer A1 - Oskinova, Lidia M. A1 - Shenar, Tomer A1 - Marchant Campos, Pablo A1 - Eldridge, J. J. A1 - Sander, Andreas Alexander Christoph A1 - Hamann, Wolf-Rainer A1 - Langer, Norbert A1 - Todt, Helge Tobias T1 - Observational properties of massive black hole binary progenitors JF - Astronomy and astrophysics : an international weekly journal N2 - Context: The first directly detected gravitational waves (GW 150914) were emitted by two coalescing black holes (BHs) with masses of ≈ 36 M⊙ and ≈ 29 M⊙. Several scenarios have been proposed to put this detection into an astrophysical context. The evolution of an isolated massive binary system is among commonly considered models. Aims: Various groups have performed detailed binary-evolution calculations that lead to BH merger events. However, the question remains open as to whether binary systems with the predicted properties really exist. The aim of this paper is to help observers to close this gap by providing spectral characteristics of massive binary BH progenitors during a phase where at least one of the companions is still non-degenerate. Methods: Stellar evolution models predict fundamental stellar parameters. Using these as input for our stellar atmosphere code (Potsdam Wolf-Rayet), we compute a set of models for selected evolutionary stages of massive merging BH progenitors at different metallicities. Results: The synthetic spectra obtained from our atmosphere calculations reveal that progenitors of massive BH merger events start their lives as O2-3V stars that evolve to early-type blue supergiants before they undergo core-collapse during the Wolf-Rayet phase. When the primary has collapsed, the remaining system will appear as a wind-fed high-mass X-ray binary. Based on our atmosphere models, we provide feedback parameters, broad band magnitudes, and spectral templates that should help to identify such binaries in the future. Conclusions: While the predicted parameter space for massive BH binary progenitors is partly realized in nature, none of the known massive binaries match our synthetic spectra of massive BH binary progenitors exactly. Comparisons of empirically determined mass-loss rates with those assumed by evolution calculations reveal significant differences. The consideration of the empirical mass-loss rates in evolution calculations will possibly entail a shift of the maximum in the predicted binary-BH merger rate to higher metallicities, that is, more candidates should be expected in our cosmic neighborhood than previously assumed. KW - gravitational waves KW - binaries: close KW - stars: early-type KW - stars: atmospheres KW - stars: winds KW - outflows KW - stars: mass-loss Y1 - 2018 U6 - https://doi.org/10.1051/0004-6361/201731449 SN - 1432-0746 VL - 609 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Fulmer, Leah M. A1 - Gallagher, John S. A1 - Hamann, Wolf-Rainer A1 - Oskinova, Lidia M. A1 - Ramachandran, Varsha T1 - Testing massive star evolution, star-formation history, and feedback at low metallicity BT - photometric analysis of OB stars in the SMC Wing JF - Astronomy and astrophysics : an international weekly journal N2 - Context. The supergiant ionized shell SMC-SGS 1 (DEM 167), which is located in the outer Wing of the Small Magellanic Cloud (SMC), resembles structures that originate from an energetic star-formation event and later stimulate star formation as they expand into the ambient medium. However, stellar populations within and surrounding SMC-SGS 1 tell a different story. Aims. We present a photometric study of the stellar population encompassed by SMC-SGS 1 in order to trace the history of such a large structure and its potential influence on star formation within the low-density, low-metallicity environment of the SMC. Methods. For a stellar population that is physically associated with SMC-SGS 1, we combined near-ultraviolet (NUV) photometry from the Galaxy Evolution Explorer with archival optical (V-band) photometry from the ESO Danish 1.54 m Telescope. Given their colors and luminosities, we estimated stellar ages and masses by matching observed photometry to theoretical stellar isochrone models. Results. We find that the investigated region supports an active, extended star-formation event spanning similar to 25-40 Myr ago, as well as continued star formation into the present. Using a standard initial mass function, we infer a lower bound on the stellar mass from this period of similar to 3 x 10(4) M-circle dot, corresponding to a star-formation intensity of similar to 6 x 10(-3) M-circle dot kpc(-2) yr(-1). Conclusions. The spatial and temporal distributions of young stars encompassed by SMC-SGS 1 imply a slow, consistent progression of star formation over millions of years. Ongoing star formation, both along the edge and interior to SMC-SGS 1, suggests a combined stimulated and stochastic mode of star formation within the SMC Wing. We note that a slow expansion of the shell within this low-density environment may preserve molecular clouds within the volume of the shell, leaving them to form stars even after nearby stellar feedback expels local gas and dust. KW - galaxies KW - stellar content KW - stars KW - formation KW - individual KW - Small KW - Magellanic Cloud Y1 - 2020 U6 - https://doi.org/10.1051/0004-6361/201834314 SN - 0004-6361 SN - 1432-0746 VL - 633 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Toalá, Jesús Alberto A1 - Bowman, Dominic A1 - Van Reeth, Timothy A1 - Todt, Helge Tobias A1 - Dsilva, Karan A1 - Shenar, Tomer A1 - Koenigsberger, Gloria Suzanne A1 - Estrada-Dorado, Sandino A1 - Oskinova, Lidia M. A1 - Hamann, Wolf-Rainer T1 - Multiple variability time-scales of the early nitrogen-rich Wolf-Rayet star WR 7 JF - Monthly notices of the Royal Astronomical Society N2 - We present the analysis of the optical variability of the early, nitrogen-rich Wolf-Rayet (WR) star WR 7. The analysis of multisector Transiting Exoplanet Survey Satellite (TESS) light curves and high-resolution spectroscopic observations confirm multiperiodic variability that is modulated on time-scales of years. We detect a dominant period of 2.6433 +/- 0.0005 d in the TESS sectors 33 and 34 light curves in addition to the previously reported high-frequency features from sector 7. We discuss the plausible mechanisms that may be responsible for such variability in WR 7, including pulsations, binarity, co-rotating interaction regions (CIRs), and clumpy winds. Given the lack of strong evidence for the presence of a stellar or compact companion, we suggest that WR 7 may pulsate in quasi-coherent modes in addition to wind variability likely caused by CIRs on top of stochastic low-frequency variability. WR 7 is certainly a worthy target for future monitoring in both spectroscopy and photometry to sample both the short (less than or similar to 1 d) and long (greater than or similar to 1000 d) variability time-scales. KW - stars: atmospheres KW - stars: evolution KW - stars: individual: WR 7 KW - stars: winds KW - outflows KW - stars: Wolft-Rayet Y1 - 2022 U6 - https://doi.org/10.1093/mnras/stac1455 SN - 0035-8711 SN - 1365-2966 VL - 514 IS - 2 SP - 2269 EP - 2277 PB - Oxford University Press CY - Oxford ER - TY - JOUR A1 - Oskinova, Lidia M. A1 - Schaerer, Daniel T1 - Ionization of He II in star-forming galaxies by X-rays from cluster winds and superbubbles JF - Astronomy and astrophysics : an international weekly journal N2 - The nature of the sources powering nebular He II emission in star-forming galaxies remains debated, and various types of objects have been considered, including Wolf-Rayet stars, X-ray binaries, and Population III stars. Modern X-ray observations show the ubiquitous presence of hot gas filling star-forming galaxies. We use a collisional ionization plasma code to compute the specific He II ionizing flux produced by hot gas and show that if its temperature is not too high (less than or similar to 2.5 MK), then the observed levels of soft diffuse X-ray radiation could explain He II ionization in galaxies. To gain a physical understanding of this result, we propose a model that combines the hydrodynamics of cluster winds and hot superbubbles with observed populations of young massive clusters in galaxies. We find that in low-metallicity galaxies, the temperature of hot gas is lower and the production rate of He II ionizing photons is higher compared to high-metallicity galaxies. The reason is that the slower stellar winds of massive stars in lower-metallicity galaxies input less mechanical energy in the ambient medium. Furthermore, we show that ensembles of star clusters up to similar to 10-20 Myr old in galaxies can produce enough soft X-rays to induce nebular He II emission. We discuss observations of the template low-metallicity galaxy I Zw 18 and suggest that the He II nebula in this galaxy is powered by a hot superbubble. Finally, appreciating the complex nature of stellar feedback, we suggest that soft X-rays from hot superbubbles are among the dominant sources of He II ionizing flux in low-metallicity star-forming galaxies. KW - galaxies KW - ISM KW - high-redshift KW - bubbles KW - X-rays Y1 - 2022 U6 - https://doi.org/10.1051/0004-6361/202142520 SN - 0004-6361 SN - 1432-0746 VL - 661 PB - EDP Sciences CY - Les Ulis ER - TY - THES A1 - Banerjee, Abhirup T1 - Characterizing the spatio-temporal patterns of extreme events BT - from recurrence to prediction N2 - Over the past decades, there has been a growing interest in ‘extreme events’ owing to the increasing threats that climate-related extremes such as floods, heatwaves, droughts, etc., pose to society. While extreme events have diverse definitions across various disciplines, ranging from earth science to neuroscience, they are characterized mainly as dynamic occurrences within a limited time frame that impedes the normal functioning of a system. Although extreme events are rare in occurrence, it has been found in various hydro-meteorological and physiological time series (e.g., river flows, temperatures, heartbeat intervals) that they may exhibit recurrent behavior, i.e., do not end the lifetime of the system. The aim of this thesis to develop some sophisticated methods to study various properties of extreme events. One of the main challenges in analyzing such extreme event-like time series is that they have large temporal gaps due to the paucity of the number of observations of extreme events. As a result, existing time series analysis tools are usually not helpful to decode the underlying information. I use the edit distance (ED) method to analyze extreme event-like time series in their unaltered form. ED is a specific distance metric, mainly designed to measure the similarity/dissimilarity between point process-like data. I combine ED with recurrence plot techniques to identify the recurrence property of flood events in the Mississippi River in the United States. I also use recurrence quantification analysis to show the deterministic properties and serial dependency in flood events. After that, I use this non-linear similarity measure (ED) to compute the pairwise dependency in extreme precipitation event series. I incorporate the similarity measure within the framework of complex network theory to study the collective behavior of climate extremes. Under this architecture, the nodes are defined by the spatial grid points of the given spatio-temporal climate dataset. Each node is associated with a time series corresponding to the temporal evolution of the climate observation at that grid point. Finally, the network links are functions of the pairwise statistical interdependence between the nodes. Various network measures, such as degree, betweenness centrality, clustering coefficient, etc., can be used to quantify the network’s topology. We apply the methodology mentioned above to study the spatio-temporal coherence pattern of extreme rainfall events in the United States and the Ganga River basin, which reveals its relation to various climate processes and the orography of the region. The identification of precursors associated with the occurrence of extreme events in the near future is extremely important to prepare the masses for an upcoming disaster and mitigate the potential risks associated with such events. Under this motivation, I propose an in-data prediction recipe for predicting the data structures that typically occur prior to extreme events using the Echo state network, a type of Recurrent Neural Network which is a part of the reservoir computing framework. However, unlike previous works that identify precursory structures in the same variable in which extreme events are manifested (active variable), I try to predict these structures by using data from another dynamic variable (passive variable) which does not show large excursions from the nominal condition but carries imprints of these extreme events. Furthermore, my results demonstrate that the quality of prediction depends on the magnitude of events, i.e., the higher the magnitude of the extreme, the better is its predictability skill. I show quantitatively that this is because the input signals collectively form a more coherent pattern for an extreme event of higher magnitude, which enhances the efficiency of the machine to predict the forthcoming extreme events. N2 - In den letzten Jahrzehnten hat das Interesse an ‘Extremereignissen’ aufgrund der zunehmenden Bedrohung, die klimabedingte Extreme wie Überschwemmungen, Hitzewellen, Dürren usw. für die Gesellschaft darstellen, zugenommen. Obwohl Extremereignisse in verschiedenen Disziplinen - von der Geowissenschaft bis zu den Neurowissenschaften - unterschiedlich definiert werden, werden sie hauptsächlich als dynamische Ereignisse innerhalb eines begrenzten Zeitrahmens charakterisiert, die das normale Funktionieren eines Systems beeinträchtigen. Obwohl Extremereignisse selten vorkommen, wurde festgestellt, dass verschiedene hydro-meteorologische und physiologische Zeitreihen (z. B. Stromabflussmengen, Temperaturen, Herzschlagintervalle) rekurrentes Verhalten. Das heißt, sie enden nicht an der Lebensdauer des Systems. Das Ziel dieser Arbeit ist es, fortschrittliche Methoden zur Untersuchung verschiedener Eigenschaften von Extremereignissen zu entwickeln. Eine der größten Herausforderungen bei der Analyse solcher extremen Ereignisse ist, dass sie große zeitliche Lücken aufweisen, da die Anzahl beobachteter Extremereignissen gering ist. Bestehende Zeitreihenanalysetools sind daher in der Regel nicht hilfreich, um die zugrundeliegenden Informationen zu entschlüsseln. Ich verwende die Edit-Distanz (ED) Methode, um extremeereignisähnliche Zeitreihen in ihrer unveränderten Form zu analysieren. ED ist eine spezielle Abstandsmetrik, die hauptsächlich zur Messung der Ähnlichkeit/Unähnlichkeit zwischen punktprozessähnlichen Daten entwickelt wurde. Ich kombiniere ED mit Rekurrenzplots, um die Wiederkehr-Eigenschaften von Hochwasserereignissen am Mississippi in den Vereinigten Staaten zu ermitteln. Außerdem werte ich die Wiederkehr-Eigenschaften quantitativ aus, um die deterministische Charakteristik und die serielle Abhängigkeit bei Hochwasserereignissen aufzuzeigen. Anschließend verwende ich dieses nichtlineare Ähnlichkeitsmaß(ED), um die paarweise Abhängigkeit in extremen Niederschlagsereignisreihen zu berechnen. Ich verknüpfe das Ähnlichkeitsmaß mit der Theorie komplexer Netzwerke, um das kollektive Verhalten von Klimaextremen zu untersuchen. In diesem Fall werden die Knoten durch die räumlichen Gitterpunkte des zu untersuchenden raumzeitlichen Klimadatensatzes definiert. Jeder Knoten repräsentiert eine Zeitreihe, die die zeitliche Entwicklung der Klimabeobachtung an diesem Gitterpunkt beschreibt. Schließlich sind die Netzwerkverbindungen Funktionen der paarweisen statistischen Interdependenz zwischen den Knotenpunkten. Zur Quantifizierung der Netztopologie können verschiedene Netzwerkmaße wie unter anderem der Grad, die Betweenness-Zentralität, oder der Clustering-Koeffizient verwendet werden. Wir wenden die oben erwähnte Methodik an, um das raumzeitliche Kohärenzmuster extremer Niederschlagsereignisse in den Vereinigten Staaten und im Einzugsgebiet des Ganges zu untersuchen. Die Ergebnisse zeigen, dass ein Zusammenhang zwischen dem Kohärenzmuster und verschiedenen Klimaprozessen und der Orographie der Region besteht. Die Identifizierung von Vorläufern, die mit dem Auftreten von Extremereignissen in naher Zukunft verbunden sind, ist äußerst wichtig, um die Bevölkerung auf eine bevorstehende Katastrophe vorzubereiten und potenziell resultierende Risiken zu mindern. Deshalb schlage ich ein datenbasiertes Vorhersageverfahren zur Bestimmung der Datenstrukturen vor, die typischerweise vor extremen Ereignissen auftreten. Das Verfahren basiert auf dem Echo-State Netzwerk, einem rekurrenten neuronalen Netz, das dem Reservoir-Computing zugeordnet wird. Im Gegensatz zu früheren Arbeiten, die Vorläuferstrukturen in der Variablen identifizieren, in der sich Extremereignisse manifestieren (aktive Variable), versuche ich die Strukturen anhand anderer dynamischer Variablen (passive Variablen) vorherzusagen. Diese Variablen weichen selbst nicht sonderlich von ihrem eigenen Sollzustand ab, aber sie besitzen eine Aussagekraft gegenüber den Extremereignissen. Meine Ergebnisse zeigen, dass die Qualität der Vorhersage von der Magnitude der Ereignisse abhängt, d.h. je extremer ein Ereignis ist, desto besser kann es vorhergesagt werden. Ich belege quantitativ, dass dieser Zusammenhang darauf basiert, dass die gesammelten Eingangssignale aussagekräftigere Kohärenzmuster für Extremereignisse hoher Magnitude bilden. Dies erhöht die Wirksamkeit des Ansatzes bei der Vorhersage bevorstehender Extremereignisse. KW - extreme events KW - Extremereignisse KW - floods KW - extreme precipitation KW - edit distance KW - recurrence plot KW - complex network KW - echo state network KW - Überschwemmungen KW - Extremniederschläge KW - Edit-Distanz KW - Rekurrenzplot KW - komplexes Netzwerk KW - Echo-State Netzwerk Y1 - 2022 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-559839 ER - TY - THES A1 - Novakovic-Marinkovic, Nina T1 - Optical control of bubble domains and skyrmions in thin films T1 - Optische Kontrolle von Blasendomänen und Skyrmionen in dünnen Schichten N2 - Laser induced switching offers an attractive possibility to manipulate small magnetic domains for prospective memory and logic devices on ultrashort time scales. Moreover, optical control of magnetization without high applied magnetic fields allows manipulation of magnetic domains individually and locally, without expensive heat dissipation. One of the major challenges for developing novel optically controlled magnetic memory and logic devices is reliable formation and annihilation of non-volatile magnetic domains that can serve as memory bits in ambient conditions. Magnetic skyrmions, topologically nontrivial spin textures, have been studied intensively since their discovery due to their stability and scalability in potential spintronic devices. However, skyrmion formation and, especially, annihilation processes are still not completely understood and further investigation on such mechanisms are needed. The aim of this thesis is to contribute to better understanding of the physical processes behind the optical control of magnetism in thin films, with the goal of optimizing material parameters and methods for their potential use in next generation memory and logic devices. First part of the thesis is dedicated to investigation of all-optical helicity-dependent switching (AO-HDS) as a method for magnetization manipulation. AO-HDS in Co/Pt multilayer and CoFeB alloys with and without the presence of Dzyaloshinskii-Moriya interaction (DMI), which is a type of exchange interaction, have been investigated by magnetic imaging using photo-emission electron microscopy (PEEM) in combination with X-ray magnetic circular dichroism (XMCD). The results show that in a narrow range of the laser fluence, circularly polarized laser light induces a drag on domain walls. This enables a local deterministic transformation of the magnetic domain pattern from stripes to bubbles in out-of-plane magnetized Co/Pt multilayers, only controlled by the helicity of ultrashort laser pulses. The temperature and characteristic fields at which the stripe-bubble transformation occurs has been calculated using theory for isolated magnetic bubbles, using as parameters experimentally determined average size of stripe domains and the magnetic layer thickness. The second part of the work aims at purely optical formation and annihilation of magnetic skyrmions by a single laser pulse. The presence of a skyrmion phase in the investigated CoFeB alloys was first confirmed using a Kerr microscope. Then the helicity-dependent skyrmion manipulation was studied using AO-HDS at different laser fluences. It was found that formation or annihilation individual skyrmions using AO-HDS is possible, but not always reliable, as fluctuations in the laser fluence or position can easily overwrite the helicity-dependent effect of AO-HDS. However, the experimental results and magnetic simulations showed that the threshold values for the laser fluence for the formation and annihilation of skyrmions are different. A higher fluence is required for skyrmion formation, and existing skyrmions can be annihilated by pulses with a slightly lower fluence. This provides a further option for controlling formation and annihilation of skyrmions using the laser fluence. Micromagnetic simulations provide additional insights into the formation and annihilation mechanism. The ability to manipulate the magnetic state of individual skyrmions is of fundamental importance for magnetic data storage technologies. Our results show for the first time that the optical formation and annihilation of skyrmions is possible without changing the external field. These results enable further investigations to optimise the magnetic layer to maximise the energy gap between the formation and annihilation barrier. As a result, unwanted switching due to small laser fluctuations can be avoided and fully deterministic optical switching can be achieved. N2 - Laser induziertes Schalten bietet eine attraktive Möglichkeit zur Manipulation kleiner magnetischer Domänen für zukünftige Speicher- und Logikbauteile auf ultrakurzen Zeitskalen. Darüber hinaus ermöglicht die rein optische Kontrolle der Magnetisierung ohne hohe angelegte Magnetfelder eine individuelle und lokale Manipulation magnetischer Domänen ohne teure Wärmeverluste. Eine der größten Herausforderungen bei der Entwicklung neuartiger optisch kontrollierter magnetischer Speicher- und Logikbauteile ist das zuverlässige Schreiben stabiler magnetischer Domänen, die unter Umgebungsbedingungen als Speicherbits dienen können. Magnetische Skyrmionen, topologisch nichttriviale wirbelf¨ormige Spin-Texturen, wurden seit ihrer Entdeckung aufgrund ihrer Stabilität und Skalierbarkeit in potenziellen spintronischen Bauelementen intensiv untersucht. Allerdings sind die Prozesse der Skyrmionenbildung und vor allem der Skyrmionenvernichtung noch immer nicht vollständig verstanden, so dass weitere Untersuchungen zu diesen Mechanismen erforderlich sind. Ziel dieser Arbeit ist es, zu einem besseren Verständnis der physikalischen Prozesse beizutragen, die der optischen Kontrolle magnetischer Texturen in dünnen Filmen zugrunde liegen, mit dem Ziel, die Materialparameter und Methoden für ihren potenziellen Einsatz in Speicher- und Logikbauteilen der nächsten Generation zu optimieren. Der erste Teil der Arbeit widmet sich der Untersuchung des rein optischen helizitätsabhängigen Schaltens (AO-HDS) als Methode zur Manipulation der Magnetisierung. AO-HDS wurde in Co/Pt-Multilayern und CoFeB-Legierungen mit und ohne DMI (Dzyaloshinskii-Moriya-Wechselwirkung), einer Art Austauschwechselwirkung, mittels magnetischer Bildgebung durch Photoemissions-Elektronenmikroskopie (PEEM) in Kombination mit magnetischem Röntgendichroismus (XMCD) untersucht. Die Ergebnisse zeigen, dass zirkular polarisiertes Licht in einem bestimmten Bereich der Laserfluenz einen Zug auf Domänenwände ausübt. Dies ermöglicht eine lokale deterministische Umwandlung des magnetischen Domänenmusters von Streifen zu Blasen Domänen in unmagnetisierten Co/Pt- Multilagen, die ausschließlich durch die Helizität der ultrakurzen Laserpulse gesteuert wird. Die Temperatur und die charakteristischen Felder, bei denen die Umwandlung von Streifen zu Blasen Domänen stattfindet, wurden mithilfe der Theorie für isolierte magnetische Blasen berechnet, wobei die experimentell ermittelte durchschnittliche Größe der Streifendom¨anen und die Dicke der magnetischen Schicht als Parameter verwendet wurden. Der zweite Teil der Arbeit zielt darauf ab, optimale Parameter zu ermitteln, die für das rein optische Schreiben und Löschen von magnetischen Skyrmionen in einem einzigen Laser Puls erforderlich sind. Das Vorhandensein einer Skyrmion-Phase in dafür verwendeten CoFeB-Legierungen wurde zunächst mit Hilfe eines Kerr-Mikroskops bestätigt. Dann wurde die helizitätsabhängige Skyrmion-Manipulation mittels AOHDS für verschiedene Laserfluenzen untersucht. Es zeigte sich, dass eine Schreiben oder Löschen einzelner Skyrmionen mittels AO-HDS zwar möglich ist, aber nicht immer zuverlässig, da Fluktuationen in der Laserfluenz oder Position den helizitätsabhängigen Effekt von AO-HDS leicht überschreiben können. Die experimentellen Ergebnisse und magnetischen Simulationen zeigten allerdings, dass die Schwellenwerte für die Laserfluenz zur Bildung und Vernichtung von Skyrmionen unterschiedlich sind. Für die Skyrmionenbildung wird eine höhere Fluenz benötigt, und bereits existierende Skyrmionen können durch Laser Pulse mit etwas geringerer Fluenz gelöscht werden. Dadurch bietet sich eine weitere Möglichkeit das Schreiben und Löschen von Skyrmionen durch die Laserfluenz zu kontrollieren. Mikromagnetische Simulationen liefern zusätzliche Erkenntnisse über den Schreib- und Löschmechanismus. Die Möglichkeit, den magnetischen Zustand einzelner Skyrmionen zu manipulieren, ist von grundlegender Bedeutung für magnetische Datenspeichertechnologien. Unsere Ergebnisse zeigen erstmalig, dass die optische Bildung und Vernichtung von Skyrmionen ohne Änderung des externen Feldes möglich ist. Diese Ergebnisse ermöglichen weitere Untersuchungen zur Optimierung der magnetischen Schicht, um die Energielücke zwischen Bildungs- und Vernichtungsbarriere zu maximieren. Dadurch kann unerwünschtes Schalten aufgrund kleiner Laserfluktuationen vermieden und vollständig deterministisches optisches Schalten erreicht werden. KW - Skyrmions KW - bubble domains KW - magnetism KW - Skyrmionen KW - Blasendomänen KW - Magnetismus KW - dünne Schichten KW - thin films Y1 - 2024 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-647069 ER - TY - JOUR A1 - Serrano-Munoz, Itziar A1 - Roveda, Ilaria A1 - Kupsch, Andreas A1 - Müller, Bernd R. A1 - Bruno, Giovanni T1 - Synchrotron X-ray refraction detects microstructure and porosity evolution during in-situ heat treatments JF - Materials Science and Engineering A: Structural Materials: Properties, Microstructure and Processing N2 - For the first time, synchrotron X-ray refraction radiography (SXRR) has been paired with in-situ heat treatment to monitor microstructure and porosity evolution as a function of temperature. The investigated material was a laser powder bed fusion (LPBF) manufactured AlSi10Mg, where the initial eutectic Si network is known to disintegrate and spherodize into larger particles with increasing temperature. Such alloy is also prone to ther-mally induced porosity (TIP). We show that SXRR allows detecting the changes in the Si-phase morphology upon heating, while this is currently possible only using scanning electron microscopy. SXRR also allows observing the growth of pores, usually studied via X-ray computed tomography, but on much smaller fields-of-view. Our results show the great potential of in-situ SXRR as a tool to gain in-depth knowledge of the susceptibility of any material to thermally induced damage and/or microstructure evolution over statistically relevant volumes. KW - synchrotron X-ray refraction radiography (SXRR) KW - Si network disintegration KW - thermally induced porosity (TIP) KW - laser powder bed fusion (LPBF) AlSi10Mg alloy KW - statistically relevant volumes Y1 - 2022 U6 - https://doi.org/10.1016/j.msea.2022.142732 SN - 0921-5093 SN - 1873-4936 VL - 838 PB - Elsevier CY - Lausanne ER - TY - JOUR A1 - Tönjes, Ralf A1 - Kori, Hiroshi T1 - Phase and frequency linear response theory for hyperbolic chaotic oscillators JF - Chaos : an interdisciplinary journal of nonlinear science N2 - We formulate a linear phase and frequency response theory for hyperbolic flows, which generalizes phase response theory for autonomous limit cycle oscillators to hyperbolic chaotic dynamics. The theory is based on a shadowing conjecture, stating the existence of a perturbed trajectory shadowing every unperturbed trajectory on the system attractor for any small enough perturbation of arbitrary duration and a corresponding unique time isomorphism, which we identify as phase such that phase shifts between the unperturbed trajectory and its perturbed shadow are well defined. The phase sensitivity function is the solution of an adjoint linear equation and can be used to estimate the average change of phase velocity to small time dependent or independent perturbations. These changes in frequency are experimentally accessible, giving a convenient way to define and measure phase response curves for chaotic oscillators. The shadowing trajectory and the phase can be constructed explicitly in the tangent space of an unperturbed trajectory using co-variant Lyapunov vectors. It can also be used to identify the limits of the regime of linear response. Y1 - 2022 U6 - https://doi.org/10.1063/5.0064519 SN - 1054-1500 SN - 1089-7682 VL - 32 IS - 4 PB - AIP Publishing CY - Melville ER - TY - JOUR A1 - Zheng, Chunming A1 - Tönjes, Ralf A1 - Pikovskij, Arkadij T1 - Transition to synchrony in a three-dimensional swarming model with helical trajectories JF - Physical review : E, Statistical, nonlinear and soft matter physics N2 - We investigate the transition from incoherence to global collective motion in a three-dimensional swarming model of agents with helical trajectories, subject to noise and global coupling. Without noise this model was recently proposed as a generalization of the Kuramoto model and it was found that alignment of the velocities occurs discontinuously for arbitrarily small attractive coupling. Adding noise to the system resolves this singular limit and leads to a continuous transition, either to a directed collective motion or to center-of-mass rotations. Y1 - 2021 U6 - https://doi.org/10.1103/PhysRevE.104.014216 SN - 2470-0045 SN - 2470-0053 VL - 104 IS - 1 PB - American Physical Society CY - College Park ER - TY - JOUR A1 - Tönjes, Ralf A1 - Pikovsky, Arkady T1 - Low-dimensional description for ensembles of identical phase oscillators subject to Cauchy noise JF - Physical review : E, Statistical, nonlinear and soft matter physics N2 - We study ensembles of globally coupled or forced identical phase oscillators subject to independent white Cauchy noise. We demonstrate that if the oscillators are forced in several harmonics, stationary synchronous regimes can be exactly described with a finite number of complex order parameters. The corresponding distribution of phases is a product of wrapped Cauchy distributions. For sinusoidal forcing, the Ott-Antonsen low-dimensional reduction is recovered. Y1 - 2020 U6 - https://doi.org/10.1103/PhysRevE.102.052315 SN - 2470-0045 SN - 2470-0053 VL - 102 IS - 5 PB - American Physical Society CY - College Park ER -