31 research outputs found
ΠΠΊΡΠΏΠ΅ΡΠΈΠΌΠ΅Π½ΡΠ°Π»ΡΠ½ΠΎΠ΅ ΠΎΠ±ΠΎΡΠ½ΠΎΠ²Π°Π½ΠΈΠ΅ ΡΡΡΠ°Π½ΠΎΠ²ΠΊΠΈ Π°ΡΠ΅ΡΠ°Π±ΡΠ»ΡΡΠ½ΠΎΠ³ΠΎ ΠΊΠΎΠΌΠΏΠΎΠ½Π΅Π½ΡΠ° Ρ Π½Π΅Π΄ΠΎΠΏΠΎΠΊΡΡΡΠΈΠ΅ΠΌ ΠΏΡΠΈ ΡΠ½Π΄ΠΎΠΏΡΠΎΡΠ΅Π·ΠΈΡΠΎΠ²Π°Π½ΠΈΠΈ ΠΏΠ°ΡΠΈΠ΅Π½ΡΠΎΠ² Ρ ΡΡΠΆΠ΅Π»ΠΎΠΉ ΡΡΠ΅ΠΏΠ΅Π½ΡΡ Π΄ΠΈΡΠΏΠ»Π°Π·ΠΈΠΈ
Purpose. Estimation of critical value of acetabular component uncoverage enabling its implantation without an additional support. Methods. A comparative analysis of an original method for intraoperative measurement of uncoverage space of acetabular component based on the measurement of the depth of uncovered sector with X-ray control by the same technique was carried out. Mathematical computer modeling based on the finite element techniqueand the mechanical experiment were performed. Critical values of uncoverage enabling safe primary fixation of acetabular component were estimated in designed models. Results. High rate of coincidence of direct intraoperative and postoperative measurements by radiograms was obtained, testifying to the possibility of application of this technique of uncoverage estimation at the stage of preoperative X-ray planning in patients with different degree of dysplasia. Using the finite element technique and the mechanical experiment on pelvis models, a possibility of mounting anacetabular component with moderate uncoverage within 25% without screws and with significant uncoverage to 35% with additional two screws fixation was demonstrated.Π¦Π΅Π»Ρ ΡΠ°Π±ΠΎΡΡ - ΠΎΠΏΡΠ΅Π΄Π΅Π»Π΅Π½ΠΈΠ΅ ΠΊΡΠΈΡΠΈΡΠ΅ΡΠΊΠΎΠΉ Π²Π΅Π»ΠΈΡΠΈΠ½Ρ Π½Π΅Π΄ΠΎΠΏΠΎΠΊΡΡΡΠΈΡ Π°ΡΠ΅ΡΠ°Π±ΡΠ»ΡΡΠ½ΠΎΠ³ΠΎ ΠΊΠΎΠΌΠΏΠΎΠ½Π΅Π½ΡΠ°, ΠΏΡΠΈ ΠΊΠΎΡΠΎΡΠΎΠΉ Π²ΠΎΠ·ΠΌΠΎΠΆΠ½Π° Π΅Π³ΠΎ ΠΈΠΌΠΏΠ»Π°Π½ΡΠ°ΡΠΈΡ Π±Π΅Π· ΠΈΡΠΏΠΎΠ»ΡΠ·ΠΎΠ²Π°Π½ΠΈΡ Π΄ΠΎΠΏΠΎΠ»Π½ΠΈΡΠ΅Π»ΡΠ½ΠΎΠΉ ΠΎΠΏΠΎΡΡ. ΠΠ΅ΡΠΎΠ΄Ρ. ΠΡΠΎΠ²Π΅Π΄Π΅Π½ ΡΡΠ°Π²Π½ΠΈΡΠ΅Π»ΡΠ½ΡΠΉ Π°Π½Π°Π»ΠΈΠ· ΠΎΡΠΈΠ³ΠΈΠ½Π°Π»ΡΠ½ΠΎΠ³ΠΎ ΡΠΏΠΎΡΠΎΠ±Π° ΠΈΠ½ΡΡΠ°ΠΎΠΏΠ΅ΡΠ°ΡΠΈΠΎΠ½Π½ΠΎΠ³ΠΎ ΠΈΠ·ΠΌΠ΅ΡΠ΅Π½ΠΈΡ ΠΏΠ»ΠΎΡΠ°Π΄ΠΈ Π½Π΅Π΄ΠΎΠΏΠΎΠΊΡΡΡΠΈΡ Π²Π΅ΡΡΠ»ΡΠΆΠ½ΠΎΠ³ΠΎ ΠΊΠΎΠΌΠΏΠΎΠ½Π΅Π½ΡΠ°, ΠΎΡΠ½ΠΎΠ²Π°Π½Π½ΠΎΠ³ΠΎ Π½Π° ΠΈΠ·ΠΌΠ΅ΡΠ΅Π½ΠΈΠΈ Π³Π»ΡΠ±ΠΈΠ½Ρ Π½Π΅ΠΏΠΎΠΊΡΡΡΠΎΠ³ΠΎ ΡΠ΅ΠΊΡΠΎΡΠ°, Ρ ΡΠ΅Π½ΡΠ³Π΅Π½ΠΎΠ²ΡΠΊΠΎΠΉ ΠΎΡΠ΅Π½ΠΊΠΎΠΉ ΡΠ΅ΠΌ ΠΆΠ΅ ΡΠΏΠΎΡΠΎΠ±ΠΎΠΌ. ΠΡΡΡΠ΅ΡΡΠ²Π»Π΅Π½Ρ ΠΌΠ°ΡΠ΅ΠΌΠ°ΡΠΈΡΠ΅ΡΠΊΠΎΠ΅ ΠΊΠΎΠΌΠΏΡΡΡΠ΅ΡΠ½ΠΎΠ΅ ΠΌΠΎΠ΄Π΅Π»ΠΈΡΠΎΠ²Π°Π½ΠΈΠ΅ Π½Π° ΠΎΡΠ½ΠΎΠ²Π΅ ΠΌΠ΅ΡΠΎΠ΄Π° ΠΊΠΎΠ½Π΅ΡΠ½ΡΡ
ΡΠ»Π΅ΠΌΠ΅Π½ΡΠΎΠ² ΠΈ ΠΌΠ΅Ρ
Π°Π½ΠΈΡΠ΅ΡΠΊΠΈΠΉ ΡΠΊΡΠΏΠ΅ΡΠΈΠΌΠ΅Π½Ρ. Π ΡΠ°Π·ΡΠ°Π±ΠΎΡΠ°Π½Π½ΡΡ
ΠΌΠΎΠ΄Π΅Π»ΡΡ
ΠΎΠΏΡΠ΅Π΄Π΅Π»ΡΠ»ΠΈΡΡ ΠΊΡΠΈΡΠΈΡΠ΅ΡΠΊΠΈΠ΅ Π²Π΅Π»ΠΈΡΠΈΠ½Ρ Π½Π΅Π΄ΠΎΠΏΠΎΠΊΡΡΡΠΈΡ, ΠΏΡΠΈ ΠΊΠΎΡΠΎΡΡΡ
Π²ΠΎΠ·ΠΌΠΎΠΆΠ½ΠΎ ΠΎΠ±Π΅ΡΠΏΠ΅ΡΠ΅Π½ΠΈΠ΅ Π½Π°Π΄Π΅ΠΆΠ½ΠΎΠΉ ΠΏΠ΅ΡΠ²ΠΈΡΠ½ΠΎΠΉ ΡΠΈΠΊΡΠ°ΡΠΈΠΈ Π°ΡΠ΅ΡΠ°Π±ΡΠ»ΡΡΠ½ΠΎΠ³ΠΎ ΠΊΠΎΠΌΠΏΠΎΠ½Π΅Π½ΡΠ° Π Π΅Π·ΡΠ»ΡΡΠ°ΡΡ. ΠΡΡΠ²Π»Π΅Π½Π° Π²ΡΡΠΎΠΊΠ°Ρ ΡΡΠ΅ΠΏΠ΅Π½Ρ ΡΠΎΠ²ΠΏΠ°Π΄Π΅Π½ΠΈΡ ΠΏΡΡΠΌΡΡ
ΠΈΠ½ΡΡΠ°ΠΎΠΏΠ΅ΡΠ°ΡΠΈΠΎΠ½Π½ΡΡ
ΠΈ ΠΏΠΎΡΠ»Π΅ΠΎΠΏΠ΅ΡΠ°ΡΠΈΠΎΠ½Π½ΡΡ
ΠΈΠ·ΠΌΠ΅ΡΠ΅Π½ΠΈΠΉ ΠΏΠΎ ΡΠ΅Π½ΡΠ³Π΅Π½ΠΎΠ³ΡΠ°ΠΌΠΌΠ°ΠΌ, ΡΡΠΎ ΡΠ²ΠΈΠ΄Π΅ΡΠ΅Π»ΡΡΡΠ²ΡΠ΅Ρ ΠΎ Π²ΠΎΠ·ΠΌΠΎΠΆΠ½ΠΎΡΡΠΈ ΠΏΡΠΈΠΌΠ΅Π½Π΅Π½ΠΈΡ Π΄Π°Π½Π½ΠΎΠ³ΠΎ ΠΌΠ΅ΡΠΎΠ΄Π° ΠΎΡΠ΅Π½ΠΊΠΈ Π½Π΅Π΄ΠΎΠΏΠΎΠΊΡΡΡΠΈΡ Π½Π° ΡΡΠ°ΠΏΠ΅ ΠΏΡΠ΅Π΄ΠΎΠΏΠ΅ΡΠ°ΡΠΈΠΎΠ½Π½ΠΎΠ³ΠΎ ΡΠ΅Π½ΡΠ³Π΅Π½ΠΎΠ²ΡΠΊΠΎΠ³ΠΎ ΠΏΠ»Π°Π½ΠΈΡΠΎΠ²Π°Π½ΠΈΡ Ρ ΠΏΠ°ΡΠΈΠ΅Π½ΡΠΎΠ² Ρ ΡΠ°Π·Π»ΠΈΡΠ½ΠΎΠΉ ΡΡΠ΅ΠΏΠ΅Π½ΡΡ Π΄ΠΈΡΠΏΠ»Π°Π·ΠΈΠΈ. Π‘ ΠΏΠΎΠΌΠΎΡΡΡ ΠΌΠ΅ΡΠΎΠ΄Π° ΠΊΠΎΠ½Π΅ΡΠ½ΡΡ
ΡΠ»Π΅ΠΌΠ΅Π½ΡΠΎΠ² ΠΈ ΠΌΠ΅Ρ
Π°Π½ΠΈΡΠ΅ΡΠΊΠΎΠ³ΠΎ ΡΠΊΡΠΏΠ΅ΡΠΈΠΌΠ΅Π½ΡΠ° Π½Π° ΠΌΠΎΠ΄Π΅Π»ΡΡ
ΡΠ°Π·Π° ΠΏΠΎΠΊΠ°Π·Π°Π½Π° Π²ΠΎΠ·ΠΌΠΎΠΆΠ½ΠΎΡΡΡ ΡΡΡΠ°Π½ΠΎΠ²ΠΊΠΈ Π°ΡΠ΅ΡΠ°Π±ΡΠ»ΡΡΠ½ΠΎΠ³ΠΎ ΠΊΠΎΠΌΠΏΠΎΠ½Π΅Π½ΡΠ° Ρ ΡΠΌΠ΅ΡΠ΅Π½Π½ΡΠΌ Π½Π΅Π΄ΠΎΠΏΠΎΠΊΡΡΡΠΈΠ΅ΠΌ Π² ΠΏΡΠ΅Π΄Π΅Π»Π°Ρ
25% Π±Π΅Π· Π²ΠΈΠ½ΡΠΎΠ² ΠΈ ΡΠΎ Π·Π½Π°ΡΠΈΡΠ΅Π»ΡΠ½ΡΠΌ Π½Π΅Π΄ΠΎΠΏΠΎΠΊΡΡΡΠΈΠ΅ΠΌ Π΄ΠΎ 35% Ρ Π΄ΠΎΠΏΠΎΠ»Π½ΠΈΡΠ΅Π»ΡΠ½ΠΎΠΉ ΡΠΈΠΊΡΠ°ΡΠΈΠ΅ΠΉ Π΄Π²ΡΠΌΡ Π²ΠΈΠ½ΡΠ°ΠΌΠΈ
Signatures of the slow solar wind streams from active regions in the inner corona
Some of local sources of the slow solar wind can be associated with
spectroscopically detected plasma outflows at edges of active regions
accompanied with specific signatures in the inner corona. The EUV telescopes
(e.g. SPIRIT/CORONAS-F, TESIS/CORONAS-Photon and SWAP/PROBA2) sometimes
observed extended ray-like structures seen at the limb above active regions in
1MK iron emission lines and described as "coronal rays". To verify the
relationship between coronal rays and plasma outflows, we analyze an isolated
active region (AR) adjacent to small coronal hole (CH) observed by different
EUV instruments in the end of July - beginning of August 2009. On August 1 EIS
revealed in the AR two compact outflows with the Doppler velocities V =10-30
km/s accompanied with fan loops diverging from their regions. At the limb the
ARCH interface region produced coronal rays observed by EUVI/STEREO-A on July
31 as well as by TESIS on August 7. The rays were co-aligned with open magnetic
field lines expanded to the streamer stalks. Using the DEM analysis, it was
found that the fan loops diverged from the outflow regions had the dominant
temperature of ~1 MK, which is similar to that of the outgoing plasma streams.
Parameters of the solar wind measured by STEREO-B, ACE, WIND, STEREO-A were
conformed with identification of the ARCH as a source region at the
Wang-Sheeley-Arge map of derived coronal holes for CR 2086. The results of the
study support the suggestion that coronal rays can represent signatures of
outflows from ARs propagating in the inner corona along open field lines into
the heliosphere.Comment: Accepted for publication in Solar Physics; 31 Pages; 13 Figure
Nanolocalized UV source of laser radiation
We show the results of optical nonlinear interaction of laser light with plasmonic nanostructures. Creation of a nanolocalized source of UV radiation (Ξ» = 260 nm) of the record high intensity was demonstated. Possibility of use of the source for biomedical applications was shown
Nanolocalized UV source of laser radiation
We show the results of optical nonlinear interaction of laser light with plasmonic nanostructures. Creation of a nanolocalized source of UV radiation (Ξ» = 260 nm) of the record high intensity was demonstated. Possibility of use of the source for biomedical applications was shown
Single photon transport by a moving atom through sub-wavelength hole
The results of investigation of photon transport through the subwavelength hole in the opaque screen by using single neutral atom are represented. The basis of the proposed and implemented method is the absorption of a photon by a neutral atom immediately before the subwavelength aperture, traveling of the atoms through the hole and emission of a photon on the other side of the screen. Realized method is the alternative approach to existing for photon transport through a subwavelength aperture: 1) self-sustained transmittance of a photon through the aperture according to the Betheβs model; 2) extra ordinary transmission because of surface-plasmon excitation
Single photon transport by a moving atom through sub-wavelength hole
The results of investigation of photon transport through the subwavelength hole in the opaque screen by using single neutral atom are represented. The basis of the proposed and implemented method is the absorption of a photon by a neutral atom immediately before the subwavelength aperture, traveling of the atoms through the hole and emission of a photon on the other side of the screen. Realized method is the alternative approach to existing for photon transport through a subwavelength aperture: 1) self-sustained transmittance of a photon through the aperture according to the Betheβs model; 2) extra ordinary transmission because of surface-plasmon excitation