National Library of Latvia, Riga 1989-in progress

[Early Conceptual Sketch], untitled. Digital image only of blue ink sketch on tracing paper, initialed

National Library of Latvia, Riga 1989-in progress

[Early Conceptual Sketch], untitled. Digital image only of blue ink sketch on tracing paper, initialed

National Library of Latvia, Riga 1989-in progress

[Conceptual Sketches], untitled. Digital image only of four black ink sketches on graph paper, initialed

National Library of Latvia, Riga 1989-in progress

[Conceptual Sketches], untitled. Digital image only of four black ink sketches on graph paper, initialed

National Library of Latvia, Riga 1989-in progress

[Conceptual Sketch], untitled. Digital image only of black and blue ink sketch on tracing paper, initialed

National Library of Latvia, Riga 1989-in progress

[Conceptual Sketches], untitled. Digital image only of black and blue ink sketches on tracing paper with marker coloring, initialed

National Library of Latvia, Riga 1989-in progress

[Conceptual Sketches], untitled. Digital image only of two black and blue ink sketches on tracing paper with marker coloring

National Library of Latvia, Riga 1989-in progress

[Conceptual Sketch], untitled. Digital image only of black and blue ink sketch on tracing paper with marker coloring

National Library of Latvia, Riga 1989-in progress

[Conceptual Sketches], untitled. Digital image only of two black ink sketches on tracing paper with marker coloring

Nutrients limiting the Algal Growth Potential (AGP) in the Gulf of Riga, eastern Baltic Sea, in spring and early summer 1996

In May, June and July 1996, samples wcre collected along one transect greatly influenced by river discharge (eastern side of the gulf), along one transect slightly influence by river discharge (western side), at one station Iocated in the mouth of the main river (River Daugava), at one station located in the center of the Gulf and at several nearshore locations of the western side. Ratios of rnolecular concentrations of in situ dissolved ioorganic nitrogen, phosphorus and silicon, as weIl as enrichment bioassays were llsed to dctcrrnine which nutrient (s) lirnited the potential biomass of phytoplankton. Both comparison of (NO.d-N02+NJ.L): P04 (DIN: DIP) values with Redfic1d's ratio and bioassay inspection led to the sarne conclusions. Phosphorus was clearly the nutrient most limiting for the potcntial biornass of test species in nitrogen- rich waters, which occurred in mid spring, in the upper layer of the southern-eastern part of the Gulf which is greatly influenced by river discharge. In late spring, with the decrease of the total DIN reserve, nitrogen and phosphorus showed an equallimiting role. In deeper layers of this area and out of the river plume (western side and central part of the gulf), nitrogen was the limiting nutrient. In summer, whcn river discharge was the lowest, a11 DIN concentrations but one ranged between 1.6 and 2.6 µM, and the whole area was nitrogen-limited for both the cyanobacterial and the algal test strains. In 74% of the samples for which nitrogen was the limiting nutrient, phosphorus was recorded to be the second potentially limiting nutrient. In contrast, silicon never appeared as limiting the growth potential of either Microcystis aeruginosa or Phaeodactylum tricornutum; phosphorus was the limiting nutrient when DIN: Si03 values were >1 (in May), but DIN: Si03 was <1 when nitrogen was limiting (June and July). The authors conclude that the recently reported decrease of silicon loading in coastal waters and its subsequent enhanced importance in pushing the outcome of species competition towards harmful species may not yet be the most important factor for the Gulf of Riga. Iron appeared for 12% of the tests in the list of nutrients limiting the potential biomass. Tentative results also indicated that a significant fraction of the nitrogen (~,4 µg-atom N 1(-1) taken up by Microcystis aeruginosa may have been in the form of dissolved organic nitrogen (DON). It is thus also suggested tentatively that more attention be paid to these nitrients during further research in the Gulf of Riga.

Caratteristiche principali dell'emissione di galassie a spirale

L’universo è il luogo che permette agli esseri umani di osservare i fenomeni fondamentali che regolano le leggi della fisica e della natura. La luce e quindi la radiazione elettromagnetica è ciò che gli astronomi utilizzano e studiano, per conoscere i meccanismi principali che governano la moltitudine di corpi celesti presenti nel cosmo. Tra questi le galassie a spirale, crogiolo di oggetti e fenomeni che permettono lo studio dell’evoluzione e dell’avanzamento dell’universo. In questo elaborato verranno presentate le loro peculiarità prestando attenzione alla loro morfologia, composizione e ai principali processi di emissione di radiazione andandone ad analizzare le diverse bande dello spettro elettromagnetico

Emissione di Compton inverso e applicazioni astrofisiche

L’emissione di Compton Inverso (IC) rientra nei processi di radiazione detti di diffusione (o di scattering) e riguarda l’interazione tra elettroni relativistici ad alta energia e fotoni molto meno energetici. Il meccanismo di interazione viene approssimato ad un semplice urto tra le due particelle, in seguito al quale il fotone acquista parte dell’energia cinetica dell’elettrone, venendo diffuso ed osservato a frequenza più alta e con direzione di propagazione diversa rispetto a quanto possedeva prima dell’urto. Il Compton Inverso è il meccanismo contrario della diffusione Compton, dove il fotone perde energia in seguito all’urto con l’elettrone e viene osservato a frequenze inferiori a quelle originarie. L’IC viene osservato in ambito astrofisico soprattutto in combinazione con l’emissione di sicrotrone – nella quale elettroni relativistici presenti in regioni magnetizzate vengono accelerati dal campo magnetico ed emettono radiazione – in un fenomeno detto Synchrotron Self-Compton. Esso avviene solitamente in sorgenti molto compatte nelle quali i fotoni prodotti per sincrotrone hanno maggiore possibilità di interagire nuovamente con gli elettroni che li hanno generati, venendo diffusi ad energie più elevate. L’IC viene inoltre osservato in combinazione alla diffusione Compton in un processo detto Comptonizzazione. Ciò si verifica in plasmi molto caldi e abbastanza rarefatti, nei quali si hanno innumerevoli scambi di energia tra le particelle che li compongono. La tesi comprende una prima parte introduttiva nella quale viene presentato il contesto storico di inizio Novecento nel quale si inserisce, tra gli altri, il fisico Arthur H. Compton. Successivamente, vengono spiegati nel dettaglio i principali meccanismi di diffusione con particolare attenzione all’IC. Infine, sono illustrate le applicazioni astrofisiche del Compton Inverso e alcune delle sorgenti nelle quali l’IC viene osservato in combinazione con altri processi di radiazione.

High spatial resolution spectroscopy of W51IRS 2E and IRS 2W: Two very massive young stars in early formation stages

We present K-band spectra of the near infrared counterparts to IRS 2E and IRS 2W which is associated with the ultracompact H II region W51d, both of them embedded sources in the Galactic compact H II region W51 IRS 2. The high spatial resolution observations were obtained with the laser guide star facility and Near-infrared Integral Field Spectrograph (NIFS) mounted at the Gemini-North observatory. The spectrum of the ionizing source of W51d shows the photospheric features N III ( 21155 angstrom) in emission and He II ( 21897 angstrom) in absorption which lead us to classify it as a young O3 type star. We detected CO overtone in emission at 23000 angstrom in the spectrum of IRS 2E, suggesting that it is a massive young object still surrounded by an accretion disk, probably transitioning from the hot core phase to an ultracompact H II region.

Star formation in the intragroup medium and other diagnostics of the evolutionary stages of compact groups of galaxies

Context. Compact groups of galaxies are entities that have high densities of galaxies and serve as laboratories to study galaxy interactions, intergalactic star formation and galaxy evolution. Aims. The main goal of this study is to search for young objects in the intragroup medium of seven compact groups of galaxies: HCG 2, 7, 22, 23, 92, 100 and NGC 92 as well as to evaluate the stage of interaction of each group. Methods. We used Fabry-Perot velocity fields and rotation curves together with GALEX NUV and FUV images and optical R-band and HI maps. Results. (i) HCG 7 and HCG 23 are in early stages of interaction; (ii) HCG 2 and HCG 22 are mildly interacting; and (iii) HCG 92, HCG 100 and NGC 92 are in late stages of evolution. We find that all three evolved groups contain populations of young blue objects in the intragroup medium, consistent with ages < 100 Myr, of which several are younger than < 10 Myr. We also report the discovery of a tidal dwarf galaxy candidate in the tail of NGC 92. These three groups, besides containing galaxies that have peculiar velocity fields, also show extended HI tails. Conclusions. Our results indicate that the advanced stage of evolution of a group, together with the presence of intragroup HI clouds, may lead to star formation in the intragroup medium. A table containing all intergalactic HII regions and tidal dwarf galaxies confirmed to date is appended.

Performance Model for MRC Receivers with Adaptive Modulation and Coding in Rayleigh Fading Correlated Channels with Imperfect CSIT

RTUWO Advances in Wireless and Optical Communications 2015 (RTUWO 2015). 5-6 Nov Riga, Latvia.