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تسجيل مستخدم جديدEta Carinaes 2014.6 Spectroscopic Event: The Extraordinary He II and N II Features
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Eta Carinaes spectroscopic events (periastron passages) in 2003, 2009, and 2014 differed progressively. He II 4687 and nearby N II multiplet 5 have special significance because they respond to very soft X-rays and the ionizing UV radiation field (EUV). HST/STIS observations in 2014 show dramatic increases in both features compared to the previous 2009.1 event. These results appear very consistent with a progressive decline in the primary wind density, proposed years ago on other grounds. If material falls onto the companion star near periastron, the accretion rate may now have become too low to suppress the EUV
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Aims. Every 5.5 years eta Cars light curve and spectrum change remarkably across all observed wavelength bands. We compare the recent spectroscopic event in mid-2014 to the events in 2003 and 2009 and investigate long-term trends. Methods. Eta Car wa
s observed with HST STIS, VLT UVES, and CTIO 1.5m CHIRON for a period of more than two years in 2012-2015. Archival observations with these instruments cover three orbital cycles. Results. Important spectroscopic diagnostics show significant changes in 2014 compared to previous events. While the timing of the first HeII 4686 flash was remarkably similar to previous events, the HeII equivalent widths were slightly larger and the line flux increased compared to 2003. The second HeII peak occurred at about the same phase as in 2009, but was stronger. The HeI line flux grew in 2009-2014 compared to 1998-2003. On the other hand, Halpha and FeII lines show the smallest emission strengths ever observed. Conclusions. The basic character of the spectroscopic events has changed in the past 2-3 cycles; ionizing UV radiation dramatically weakened during each pre-2014 event but not in 2014. The strengthening of HeI emission and the weakening of the lower-excitation wind features in our direct line of sight implies a substantial change in the physical parameters of the emitting regions. The polar spectrum at FOS4 shows less changes in the broad wind emission lines, which may be explained by the latitude-dependent wind structure of eta Car. The quick and strong recovery of the HeII emission in 2014 supports a scenario, in which the wind-wind shock may not have completely collapsed as was proposed for previous events. All this may be the consequence of just one elementary change, namely a strong decrease in the primarys mass-loss rate.
We report the detection of the emission line He II 4686 A in eta Carinae. The equivalent width of this line is ~100 mA along most of the 5.5-yr cycle and jumps to ~900 mA just before phase 1.0, followed by a brief disappearance. The similarity betwee
n the intensity variations of this line and of the X-ray light curve is remarkable, suggesting that they are physically connected. We show that the number of ionizing photons in the ultraviolet and soft X-rays, expected to be emitted in the shock wave from the colliding winds, is of the order of magnitude required to produce the He II emission via photoionization. The emission is clearly blueshifted when the line is strong. The radial velocity of the line is generally -100 Km/s, decreases steadily just before the event, and reaches -400 Km/s at ph = 1.001. At this point, the velocity gradient suddenly changes sign, at the same time that the emission intensity drops to nearly zero. Possible scenarios for explaining this emission are briefly discussed. The timing of the peak of He II intensity is likely to be associated to the periastron and may be a reliable fiduciary mark, important for constraining the orbital parameters.
We present multi-epoch photometry and spectroscopy of a light echo from eta Carinaes 19th century Great Eruption. This echo shows a steady decline over a decade, sampling the 1850s plateau of the eruption. Spectra show the bulk outflow speed increasi
ng from 150 km/s at early times, up to 600 km/s in the plateau. Later phases also develop remarkably broad emission wings indicating mass accelerated to more than 10,000 km/s. Together with other clues, this provides direct evidence for an explosive ejection. This is accompanied by a transition from narrow absorption lines to emission lines, often with broad P Cygni profiles. These changes imply that the pre-1845 luminosity spikes are distinct from the 1850s plateau. The key reason for this change may be that shock interaction dominates the plateau. The spectral evolution of eta Car closely resembles that of UGC2773-OT, which had clear signatures of shock interaction. We propose a 2-stage scenario for eta Cars eruption: (1) a slow outflow in the decades before the eruption, driven by binary interaction that produced a dense equatorial outflow, followed by (2) explosive energy injection that drove CSM interaction, powering the plateau and sweeping slower CSM into a fast shell that became the Homunculus. We discuss how this sequence could arise from a stellar merger in a triple system, leaving the eccentric binary seen today. This gives a self-consistent scenario that may explain interacting transients across a wide range of initial mass.
The periodic spectroscopic events in eta Carinae are now well established and occur near the periastron passage of two massive stars in a very eccentric orbit. Several mechanisms have been proposed to explain the variations of different spectral feat
ures, such as an eclipse by the wind-wind collision boundary, a shell ejection from the primary star or accretion of its wind onto the secondary. All of them have problems explaining all the observed phenomena. To better understand the nature of the cyclic events, we performed a dense monitoring of eta Carinae with 5 Southern telescopes during the 2009 low excitation event, resulting in a set of data of unprecedented quality and sampling. The intrinsic luminosity of the He II 4686 emission line (L~310 Lsun) just before periastron reveals the presence of a very luminous transient source of extreme UV radiation emitted in the wind-wind collision (WWC) region. Clumps in the primarys wind probably explain the flare-like behavior of both the X-ray and He II 4686 light-curves. After a short-lived minimum, He II 4686 emission rises again to a ne
We report on H-alpha spectroscopy of the 2009.0 spectroscopic event of eta Carinae collected via SMARTS observations using the CTIO 1.5 m telescope and echelle spectrograph. Our observations were made almost every night over a two month interval arou
nd the predicted minimum of eta Car. We observed a significant fading of the line emission that reached a minimum seven days after the X-ray minimum. About 17 d prior to the H-alpha flux minimum, the H-alpha profile exhibited the emergence of a broad, P Cygni type, absorption component (near a Doppler shift of -500 km/s) and a narrow absorption component (near -144 km/s and probably associated with intervening gas from the Little Homunculus Nebula). All these features were observed during the last event in 2003.5 and are probably related to the close periastron passage of the companion. We argue that these variations are consistent with qualitative expectations about changes in the primary stars stellar wind that result from the wind-wind collision with a massive binary companion and from atmospheric eclipses of the companion.
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