Karaokeilmiö

Only abstract. Paper copies of master’s theses are listed in the Helka database (http://www.helsinki.fi/helka). Electronic copies of master’s theses are either available as open access or only on thesis terminals in the Helsinki University Library.Vain tiivistelmä. Sidottujen gradujen saatavuuden voit tarkistaa Helka-tietokannasta (http://www.helsinki.fi/helka). Digitaaliset gradut voivat olla luettavissa avoimesti verkossa tai rajoitetusti kirjaston opinnäytekioskeilla.Endast sammandrag. Inbundna avhandlingar kan sökas i Helka-databasen (http://www.helsinki.fi/helka). Elektroniska kopior av avhandlingar finns antingen öppet på nätet eller endast tillgängliga i bibliotekets avhandlingsterminaler.Tässä kvalitatiivisessa tutkimuksessa selvitetään, mikä saa ihmiset julkisesti laulamaan. Mitä eri toimijat karaokessa arvostavat, ja mitkä ovat heidän osallistumismotiivinsa? Tutkimuksessa keskitytään pääasiassa yhden lahtelaisen ravintolan, Ten Dollars Saluunan, karaokeiltojen ja kävijöihin. Syitä etsitään tarkastelemalla karaokeiltaan osallistujien käyttäytymisen perusteita sekä karaoken sosiaaliseen maailmaan liittyviä erityispiirteitä. Tutkimus on tehty havainnoimalla karaokeiltoja sekä kohderavintolassa että muissa lahtelaisissa karaokeravintoloissa. Tutkimusta varten on myös haastateltu karaokeillan osallistujia, sekä järjestäjiä että asiakkaita. Aineisto on analysoitu kvalitatiivisen sisältöanalyysin menetelmin. Aineistoon kuuluu myös aiemmin tehty teemahaastattelu sekä aiemmat havainnot karaokeilloista eripuolilla Suomea. Työssä tukeudun myös muutamaan suomalaisesta karaokesta tehtyyn opinnäytetyöhön sekä lehtiartikkeleihin. Karaoke on japania, ja se merkitsee ”orkesteriäänitettä ilman vokaalilaulua”. Suomalaisen karaokevetäjän sanoin karaoke on laulamista ”bändinkorvikkeelle”. Karaokessa laulaja laulaa kuvalevyltä soitettavan säestyksen tahdissa. Joissakin tutkimuksissa käytetty määritelmä ”tyhjä orkesteri” on käännösvirhe, joka antaa karaokesta harhaanjohtavan kuvan. Suomessa karaokea lauletaan pääsiassa ravintolassa, mutta myös yksityisissä tilaisuuksissa. Karaoke on enemmän kuin japanilainen keksintö. Se on samalla sosiaalinen innovaatio, joka on levinnyt ympäri maailman. Se on globaali-ilmiö, johon liittyy kulttuurillisia erityispiirteitä. Karaoke on sopeutunut parhaiten maihin, joissa on vankka yhteisölauluperinne. Suomalaisen karaoken erityispiirteisiin kuuluvat karaoken kirjoittamattomat säännöt, jotka ovat sekä yleisiä että vetäjäkohtaisia. Säännöt tukevat karaokelaulajan julkista esiintymistä. Säännöillä pyritään myös minimoimaan kilpailutilanteen syntyminen laulajien välille. Karaokevetäjällä on suuri merkitys karaokeillan ilmapiirin luojana. Karaoken arvot ovat syntyneet sosiaalisissa tilanteissa, joissa osallistujat toimivat suhteessa johonkin itsensä ulkopuolella olevaan. Karaoke vaikuttaa olevan yhteisöllisiä tunteita herättävää ja tukevaa sosiaalista toimintaa parhaimmillaan. Karaokeen liittyy sekä hauskuus että vakavuus. Laulaminen on itsensä kehittämistä ja pätemistä itselleen. Laulajat käsittelevät emootioitaan laulaessaan. Laulunsanoitukset toimivat tunteiden tulkkina. Karaokea lauletaan esiintymispelon voittamiseksi. Laulamalla halutaan herättää yleisön huomiota. Kannustaminen koetaan itsetuntoa kohottavana. Karaokelaulajat voidaan jakaa karkeasti esiintyjiin, harrastajiin ja pelleilijöihin eli näkyvässä humalassa esiintyviin. Esiintyjät kiertävät eri ravintoloissa tuomassa itseään julki. Harrastajat kulkevat mieluiten saman karaokevetäjän illoissa. Pelleilijät eivät laula, vaan tavoittelevat humalaista vitsikkyyttä, joka ei yleisöä kuitenkaan viihdytä. Pelleilijöiden osuus on vähentynyt alkuaikojen karaokesta. Yhä useammat karaokelaulajat laulavat selvinpäin. Kulttuurisosiologisena ravintolatutkimuksena työ nojaa Pertti Alasuutarin pienyhteisötutkimukseen. Aihetta on myös pohdittu Erik Allardtin esittämien käyttäytymistä ohjaavan valintateorian pohjalta. Muita käytettyjä käsitteitä ovat Erving Goffmanin näyttämöt ja Unruhin sosiaaliset maailmat ja George Meadin "self" eli minäkuva

Earth Trojan asteroids: A study in support of observational searches

Observational searches for asteroids orbiting near Earth's triangular Lagrange points face unique obstacles. A population of such asteroids would occupy a large projected area on the sky (possibly hundreds of square degrees) and is not favorably placed with respect to the Sun. Here we examine the properties of synthetic populations of Earth ``Trojans'' in order to aid in the optimization of observational searches for them. We find that the highest on-sky projected number densities are not located at the positions of the L4 and L5 points themselves, but rather a few degrees closer to the Sun. Also, asteroids on orbits about the L4 and L5 points typically brighten as the difference between their ecliptic longitude and that of the Sun increases owing to phase effects, but their number density on the sky concurrently falls rapidly.Comment: 20 pages, 5 figures and 3 tables. Submitted to Icaru

Anisotropies in the interplanetary intensity of solar protons E sub p 0.3 MeV

From the data on solar protons with energy 0.3 MeV obtained by Explorer 35 since July 1967, ten events were selected for the study of intensity vs time and of angular distributions of intensity in interplanetary space near the earth. The bases of selection were that the events be of adequate intensity for statistically satisfactory study and that they be attributable to a single solar flare so that their time histories were not complicated by overlapping emissions of particles. The principal findings for these events are presented

The 1990 MB: The first Mars Trojan

Asteroid 1990 MB was discovered by D. H. Levy and H. E. Holt during the course of the Mars and Earth Crossing Asteroid and Comet Survey. An orbit based on a 9 day arc and the asteroid's location near Mars' L5 (trailing Lagrangean) longitude led E. Boswell to speculate that it might be in 1:1 resonance with Mars, analogous to the Trojan asteroids of Jupiter. Subsequent observations strengthened the possibility, and later calculations confirmed it. Thus 1990 MB is the first known asteroid in 1:1 resonance with a planet other than Jupiter. The existence of 1990 MB (a small body most likely between 2 and 4 km in diameter) provides remarkable confirmation of computer simulations. These self consistent n-body simulations demonstrated this sort of stability for Trojans of all the terrestrial planets over at least a 2 million year time base. The discovery of 1990 MB suggests that others of similar or smaller diameter may be found. Using hypothetical populations of Mars Trojans, their possible sky plane distributions were modeled as a first step in undertaking a systematic observational search of Mars' L4 and L5 libration regions

Asteroids in the Inner Solar System I - Existence

Ensembles of in-plane and inclined orbits in the vicinity of the Lagrange points of the terrestrial planets are integrated for up to 100 million years. The integrations incorporate the gravitational effects of Sun and the eight planets (Pluto is neglected). Mercury is the least likely planet, as it is unable to retain tadpole orbits over 100 million year timescales. Both Venus and the Earth are much more promising, as they possess rich families of stable tadpole and horseshoe orbits. Our survey of Trojans in the orbital plane of Venus is undertaken for 25 million years. Some 40% of the survivors are on tadpole orbits. For the Earth, the integrations are pursued for 50 million years. The stable zones in the orbital plane are larger for the Earth than for Venus, but fewer of the survivors are tadpoles. Both Venus and the Earth also have regions in which inclined test particles can endure near the Lagrange points. For Venus, only test particles close to the orbital plane are stable. For the Earth, there are two bands of stability, one at low inclinations (i < 16 degrees) and one at moderate inclinations (between 24 degrees and 34 degrees). The inclined test particles that evade close encounters are primarily moving on tadpole orbits. Our survey of in-plane test particles near the Martian Lagrange points shows no survivors after 60 million years. Low inclination test particles do not persist, as their inclinations are quickly increased until the effects of a secular resonance with Jupiter cause de-stabilisation. Numerical integrations of inclined test particles for timespans of 25 million years show stable zones for inclinations between 14 and 40 degrees.Comment: 20 pages, 21 figures, Monthly Notices (in press

Eccentricities of Planets in Binary Systems

The most puzzling property of the extrasolar planets discovered by recent radial velocity surveys is their high orbital eccentricities, which are very difficult to explain within our current theoretical paradigm for planet formation. Current data reveal that at least 25% of these planets, including some with particularly high eccentricities, are orbiting a component of a binary star system. The presence of a distant companion can cause significant secular perturbations in the orbit of a planet. At high relative inclinations, large-amplitude, periodic eccentricity perturbations can occur. These are known as "Kozai cycles" and their amplitude is purely dependent on the relative orbital inclination. Assuming that every planet host star also has a (possibly unseen, e.g., substellar) distant companion, with reasonable distributions of orbital parameters and masses, we determine the resulting eccentricity distribution of planets and compare it to observations? We find that perturbations from a binary companion always appear to produce an excess of planets with both very high (e>0.6) and very low (e<0.1) eccentricities. The paucity of near-circular orbits in the observed sample implies that at least one additional mechanism must be increasing eccentricities. On the other hand, the overproduction of very high eccentricities observed in our models could be combined with plausible circularization mechanisms (e.g., friction from residual gas) to create more planets with intermediate eccentricities (e=0.1-0.6).Comment: 8 pages, to appear in "Close Binaries in the 21st Century: New Opportunities and Challenges", ed. A. Gimenez et al. (Springer

On the origin of eccentricities among extrasolar planets

Most observed extrasolar planets have masses similar to, but orbits very different from, the gas giants of our solar system. Many are much closer to their parent stars than would have been expected and their orbits are often rather eccentric. We show that some of these planets might have formed in systems much like our solar system, i.e. in systems where the gas giants were originally on orbits with a semi-major axis of several au, but where the masses of the gas giants were all rather similar. If such a system is perturbed by another star, strong planet-planet interactions follow, causing the ejection of several planets while leaving those remaining on much tighter and more eccentric orbits. The eccentricity distribution of these perturbed systems is very similar to that of the observed extrasolar planets with semi-major axis between 1 and 6 au.Comment: Accepted for publication in MNRAS Letter

The role of cluster evolution in disrupting planetary systems and disks: the Kozai mechanism

We examine the effects of dynamical evolution in clusters on planetary systems or protoplanetary disks orbiting the components of binary stars. In particular, we look for evidence that the companions of host stars of planetary systems or disks could have their inclination angles raised from zero to between the threshold angles (39.23 degrees and 140.77 degrees) that can induce the Kozai mechanism. We find that up to 20 per cent of binary systems have their inclination angles increased to within the threshold range. Given that half of all extrasolar planets could be in binary systems, we suggest that up to 10 per cent of extrasolar planets could be affected by this mechanism.Comment: 5 pages, 4 figures, accepted for publication in MNRAS. References update