90.00.00 GEOPHYSICS, ASTRONOMY, AND ASTROPHYSICS (for more detailed headings, see the Geophysics Appendix)
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Context. In active galaxies, matter is accreted onto super massive black holes (SMBH). This accretion process causes a region roughly the size of our solar system to outshine the entire host galaxy, forming an active galactic nucleus (AGN). In some of these active galaxies, highly relativistic particle jets are formed parallel to the rotation axis of the super massive black hole. A fraction of these sources is observed under a small inclination angle between the pointing direction of the jet and the observing line of sight. These sources are called blazars. Due to the small inclination angle and the highly relativistic speeds of the particles in the jet, beaming effects occur in the radiation of these particles. Blazars can be subdivided into the high luminosity flat spectrum radio quasars (FSRQs) and the low luminosity BL Lacertae objects (BL Lacs). As all AGN, blazars are broadband emitters and therefore observable from the longest wavelengths in the radio regime to the shortest wavelengths in the gamma-ray regime. In this thesis I will analyze blazars at these two extremes with respect to their parsec-scale properties in the radio and their time evolution properties in gamma-ray flux.
Method. In the radio regime the technique of very long baseline interferometry (VLBI) can be used in order to spatially resolve the synchrotron radiation coming from those objects down to sub-parsec scales. This information can be used to observe the time evolution of the structure of such sources. This is done in large monitoring programs such as the MOJAVE (15 GHz) and the Boston University blazar monitoring program (43 GHz). In this thesis I utilize data of 28 sources from these monitoring programs spanning 10 years of observation from 2003 to 2013, resulting in over 1800 observed epochs, to study the brightness temperature and diameter gradients of these jets. I conduct a search for systematic geometry transitions in the radio jets. The synchrotron cooling time in the radio core of the jets is used to determine the magnetic field strength in the radio core. Considering the jet geometry, these magnetic field strengths are scaled to the ergosphere of the SMBH in order to obtain the distance of the radio core to the SMBH.
In the gamma-regime these blazars cannot be spatially resolved. Due to this, it is hard to put strong constrains onto where the gamma-ray emitting region is. Blazars have shown to be variable at high energies on time scales down to minutes. The nature of this variability can be studied in order to put constrains on the particle acceleration mechanism and possibly the region and size of the gamma-ray emitting region. The variability of blazars in the energy range between 0.1 GeV and 1 GeV can for example be observed with the pair-conversion telescope on board the Fermi satellite. I use 10 years of data from the Fermi-LAT (LAT: Large Area Telescope) satellite in order to study the variability of a large sample of blazars (300-800, depending on the used significance filters for data points). I quantify this variability with the Ornstein-Uhlenbeck (OU) parameters and the power spectral density (PSD) slopes. The same procedure is applied to 20 light curves available for the radio sample.
Results. The diameter evolution along the jet axis of the radio sources suggests, that FSRQs feature flatter gradients than BL Lacs. Fitting these gradients, it is revealed that BL Lacs are systematically better described by a simple single power law than FSRQs. I found 9 sources with a strongly constrained geometry transition. The sources are 0219+421, 0336-019, 0415+379, 0528+134, 0836+710, 1101+384, 1156+295, 1253-055 and 2200+420. In all of these sources, the geometry transition regions are further out in the jet than the Bondi sphere. The magnetic field strengths of BL Lacs is systematically larger than that of FSRQs. However the scaling of these fields suggest that the radio cores of BL Lac objects are closer to the SMBHs than the radio cores of FSRQs. Analyzing the variability of Fermi-LAT light curves yields consistent results for all samples. FSRQs show systematically steeper PSD slopes and feature OU parameters more favorable to strong variability than BL Lacs. The Fermi-LAT light curves of the sub-sample of radio jets, suggest an anticorrelation between the jet complexity from the radio observations and the OU-parameters as well as the PSD slopes from the gamma-ray observations.
Conclusion.
The flatter diameter gradients of FSRQs suggest that these sources are more collimated further down the jet than BL Lacs. The systematically better description of the diameter and brightness temperature gradient by a single power law of BL Lacs, suggest that FSRQs are more complex with respect to the diameter evolution along the jet and the surface brightness distribution than BL Lac objects. FSRQs often feature regions where recollimation can occur in distinct knots within the jets. For the sources where a geometry transition could be constrained, the Bondi radius, being systematically smaller than the position of the transition region along the jet axis, suggest that changing pressure gradients are not the sole cause for these systematic geometry transitions. Nevertheless they may be responsible for recollimation regions, found typically downstream the jet, beyond the Bondi radius and the transition zone. The difference in the distance of the radio cores between FSRQs and BL Lacs is most likely due to the combination of differences in SMBH masses and systematically smaller jet powers in BL Lacs. The variability in energy ranges above 100 MeV and above 1 GeV-regime suggest that many light curves of BL Lac objects are more likely to be white noise while the PSD slopes and the OU parameters of FSRQ gamma-ray light curves favor stronger variability on larger time scales with respect to the time binning of the analyzed light curve. Although the anticorrelation of the jet complexity acquired from the radio observations and the PSD slopes and OU parameters from the gamma-observations suggest that more complex sources favor OU parameters and PSD slopes resulting in more variability (not white noise) it is beyond the scope of this thesis to pinpoint whether this correlation results from causation. The question whether a complex jet causes more gamma-ray variability or more gamma-ray variability causes more complex jets cannot be answered at this point. Nevertheless the computed correlation measures suggest that this dependence is most likely not linear and therefore an indication that these effects might even interact.
Active galactic nuclei (AGNs) are among the brightest sources in our universe. These galaxies are considered active because their central region is brighter than the luminosities of all stars in a galxies can provide. In their center is a supermassive black hole (SMBH) surrounded by an accretion disk and further out a dusty torus. AGN can be found with emission over the whole electromagnetic spectrum, starting at radio frequencies over optical and X-ray emission up to the $\gamma$-rays. Not all of these sources are detected in each frequency regime. In this work mainly blazars are examined at low radio frequencies. Blazars are a subclass of radio-loud AGN. These radio-loud sources usually exhibit highly collimated jets perpendicular to the accretion disk. For blazars these jets are pointed in the direction of the observer and their emission is highly variable. \\
AGN are classified in different subclasses based on their morphology. These different subclasses are combined in the AGN unification model, which explains the different morphologies by having sources only varying in their luminosities and their angle to the line of sight to the observer. Blazars are these targets, where the jet is pointing towards the observer, while the AGN observed edge on are called radio galaxies. This means that blazars should be the counterparts to radio galaxies seen from a different angle. Testing this is one of the goals in this work. \\
After the discovery of AGN in the 1940s these objects have been studied at all wavelengths. With the development of interferometry with radio telescopes the angular resolution for radio observations could be improved. In the last 20 years many AGN are regularly monitored. One of these monitoring programs is the MOJAVE program, monitoring 274 AGNs with using the Very Long Baseline Interferometry (VLBI) technique. The monitoring provides information on the evolution and structure of AGN and their jets. However, the mechanisms of the jet formation and their collimation are not fully understood. Due to relativistic effects it is difficult to obtain intrinsic instead of apparent parameters of these jets. One approach to get closer to the intrinsic jet power is by observing the regions, in which the jets end and interact with the intergalactic medium. Observations at lower radio frequencies are more sensitive for extended diffuse emission. \\
Since December 2012 a new radio telescope for low frequencies is observing. It is a telescope with stations consisting of dipole antennas. The major part of the array located in the Netherlands (38 stations) with 12 additional international stations in Germany, France, Sweden, Poland and the United Kingdom. This instrument is called the Low Frequency Array (LOFAR). LOFAR offers the possibility to observe at frequencies between 30--250 MHz in combination with angular resolution (below 1 arcsec for the full array), which was not available with previous telescopes. \\
In this work results of blazar studies with LOFAR observations are presented. To take advantage of a large database with multi-wavelength observations and kinematic studies the MOJAVE 1.5 Jy flux limited sample was chosen. Based on the preliminary results of the LOFAR Multifrequency Snapshot Sky Survey (MSSS) the flux densities and spectral indices of blazars of the MOJAVE sample are examined. 125 counterparts of MOJAVE blazars were found in the MSSS catalog. Since the MSSS observations only contain the stations in the Netherlands and observes in snapshots, the angular resolution and the sensitivity is limited. The first MSSS catalog was produced with an angular resolution of $\sim$120 arcsec and a sensitivity of $\sim$50--100 mJy. Another advantage of the MOJAVE sample is the monitoring of these sources with the Owens Valley Radio Observatory (OVRO) at 15 GHz to produce radio lightcurves. With these observations it is possible to get quasi-simultaneous flux densities at 15 GHz for the corresponding MSSS observations. By having quasi-simultaneous observations the variability of the blazars affects the flux densities less than with the use of archival data. The spectral indices obtained by the combination of MSSS and OVRO flux densities can be used to estimate the contribution of the diffuse extended emission for these AGNs. \\
Comparing the MSSS catalog with the OVRO data points, the flux densities have a tendency to be higher at low frequencies. This is expected due to the higher contribution of extended emission. The broadband spectral index distribution shows a peak at $\sim-0.2$. While some sources seem to have steeper spectral indices meaning that extended emission contributes a large fraction of the total flux density, more than the half of the sample shows flat spectral indices. The flat spectral indices show that the total flux densities of these sources are dominated by their relativistic beamed emission regions, which is the same for the observations at GHz frequencies. \\
To obtain more detailed images of these sources the MSSS measurement sets including sources of the sample were reprocessed to improve the angular resolution to $\sim$30 arcsec. The higher angular resolution reveals extended diffuse emission of several blazars. Since the reimaging results were not fully calibrated only the morphology at this resolution could be examined. However, with the short snapshot observations the images obtained with this strategy are affected from artifacts. The reimaging could be successfully performed for 93 sources in one frequency band. For 45 of these sources all availabe frequency bands could be reprocessed and used to created averaged images. These images are presented in this work. As a results of the reimaging process a pilot sample was defined to observe targets with diffuse extended emission using the whole LOFAR array including the international stations. \\
The second part of this work presents the results of a pilot sample consisting of four blazars observed with the LOFAR international array. Since the calibration of this kind of LOFAR observation is still in development, the main focus was the description of the used calibration strategy. The calibration strategies still has some limitation but resulted in images with angular resolutions of less than 1 arcsec. The morphology of all four blazars show features confirming the expectations of their counterpart radio galaxies. With the flux densities of the extended emission found in these brightness distributions the extended radio luminosities are calculated. Comparing these to the radio galaxy classifications also confirm the expectations from the unification model. \\
By extending the sample of observed blazars with LOFAR international in future the calibration strategy can be used to create similar high resolution images. A larger sample can be used to test the unification model with statistical significant results. \\
Classical novae are thermonuclear explosions occurring on the surface of white dwarfs.
When co-existing in a binary system with a main sequence or more evolved star, mass
accretion from the companion star to the white dwarf can take place if the companion
overflows its Roche lobe. The envelope of hydrogen-rich matter which builds on
top of the white dwarf eventually ignites under degenerate conditions, leading to
a thermonuclear runaway and an explosion in the order of 1046 erg, while leaving
the white dwarf intact. Spectral analyses from the debris indicate an abundance of
isotopes that are tracers of nuclear burning via the hot CNO cycle, which in turn
reveal some sort of mixing between the envelope and the white dwarf underneath.
The exact mechanism is still a matter of debate.
The convection and deflagration in novae develop in the low Mach number regime.
We used the Seven League Hydro code (SLH ), which employs numerical schemes
designed to correctly simulate low Mach number flows, to perform two and three-
dimensional simulations of classical novae. Based on a spherically-symmetric model
created with aid of a stellar evolution code, we developed our own nova model and
tested it on a variety of numerical grids and boundary conditions for validation. We
focused on the evolution of temperature, density and nuclear energy generation rate at
the layers between white dwarf and envelope, where most of the energy is generated,
to understand the structure of the transition region, and its effect on the nuclear
burning. We analyzed the resulting dredge-up efficiency stemming from the convective
motions in the envelope. Our models yield similar results to the literature, but seem
to depend very strongly on the numerical resolution. We followed the evolution of
the nuclear species involved in the CNO cycle and concluded that the thermonuclear
reactions primarily taking place are those of the cold and not the hot CNO cycle.
The reason behind this could be that under the conditions generally assumed for
multi-dimensional simulations, the envelope is in fact not degenerate. We performed
initial tests for 3D simulations and realized that alternative boundary conditions are
needed.