Pub Date : 2023-01-01DOI: 10.25518/0037-9565.11368
Ahmed Bougherara, Ramdane Marmi, Moussa Boulaarak, Kamel Boufaa
La vulnérabilité du site de la ville de Mila aux mouvements de masse est une contrainte majeure devant son développement urbain. Son héritage morphologique explique largement sa dynamique actuelle. Les grandes coulées quaternaires, issues du démantèlement du flanc nord de Marechau, ont dévié l’oued Mila vers l’ouest pour s’enfoncer sous forme d’arc de cercle et dégager la colline d’El Kherba. La massivité de cette dernière a permis l’installation d’une série de ravins (paléo-vallons) parallèles, inégalement creusés. Faute de soutirage efficace, ces derniers ont été comblés. La surface de contact entre la roche en place et le matériau de comblement est restée une semelle de glissement potentielle. Aussi, la fréquence et l’intensité des séismes (probablement en partie induits) sont loin d’être négligeables. En effet, après l’envahissement du site par une urbanisation rapide et massive, les effets induits des derniers séismes ont été probablement amplifiés d’où les dégâts observés.
{"title":"Le séisme de Mila du 07/08/2020 (Nord-Est algérien) : essai d’interprétation de l’activité sismique et des effets induits au niveau de la colline d’El Kherba","authors":"Ahmed Bougherara, Ramdane Marmi, Moussa Boulaarak, Kamel Boufaa","doi":"10.25518/0037-9565.11368","DOIUrl":"https://doi.org/10.25518/0037-9565.11368","url":null,"abstract":"La vulnérabilité du site de la ville de Mila aux mouvements de masse est une contrainte majeure devant son développement urbain. Son héritage morphologique explique largement sa dynamique actuelle. Les grandes coulées quaternaires, issues du démantèlement du flanc nord de Marechau, ont dévié l’oued Mila vers l’ouest pour s’enfoncer sous forme d’arc de cercle et dégager la colline d’El Kherba. La massivité de cette dernière a permis l’installation d’une série de ravins (paléo-vallons) parallèles, inégalement creusés. Faute de soutirage efficace, ces derniers ont été comblés. La surface de contact entre la roche en place et le matériau de comblement est restée une semelle de glissement potentielle. Aussi, la fréquence et l’intensité des séismes (probablement en partie induits) sont loin d’être négligeables. En effet, après l’envahissement du site par une urbanisation rapide et massive, les effets induits des derniers séismes ont été probablement amplifiés d’où les dégâts observés.","PeriodicalId":35838,"journal":{"name":"Bulletin de la Societe Royale des Sciences de Liege","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2023-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135053158","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2023-01-01DOI: 10.25518/0037-9565.11190
Callum AUBREY, Ralf NAPIWOTZKI
The origin of subdwarf B stars (sdBs) is unclear. Different formation channels are proposed including: close-binary evolution, helium-mixing on the red giant branch and the hot flasher scenario. Circumstantial evidence exists that sdBs can result from single star evolution in high metallicity populations. We investigate this possibility by using membership in the thin, thick disk and halo populations as a metallicity indicator. Radial velocity measurements were com-bined with Gaia proper motions to calculate space motions in the Galaxy. Galactic orbits and population memberships were derived. Preliminary results indicate more sdBs are members of the thin disk (86 sdBs) than of thick disk and halo (28 sdBs). Apparently single sdBs are found among all three populations. We look into the temperature distributions of the different types and discuss implication for formation scenarios.
{"title":"The origin of subdwarf B stars","authors":"Callum AUBREY, Ralf NAPIWOTZKI","doi":"10.25518/0037-9565.11190","DOIUrl":"https://doi.org/10.25518/0037-9565.11190","url":null,"abstract":"The origin of subdwarf B stars (sdBs) is unclear. Different formation channels are proposed including: close-binary evolution, helium-mixing on the red giant branch and the hot flasher scenario. Circumstantial evidence exists that sdBs can result from single star evolution in high metallicity populations. We investigate this possibility by using membership in the thin, thick disk and halo populations as a metallicity indicator. Radial velocity measurements were com-bined with Gaia proper motions to calculate space motions in the Galaxy. Galactic orbits and population memberships were derived. Preliminary results indicate more sdBs are members of the thin disk (86 sdBs) than of thick disk and halo (28 sdBs). Apparently single sdBs are found among all three populations. We look into the temperature distributions of the different types and discuss implication for formation scenarios.","PeriodicalId":35838,"journal":{"name":"Bulletin de la Societe Royale des Sciences de Liege","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2023-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135053160","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2023-01-01DOI: 10.25518/0037-9565.11278
E. J. SNOWDON, C. S. JEFFERY, S. SCHLAGENHAUF
The Southern African Large Telescope (SALT) survey of He-rich hot subdwarfs has identi-fied several binary candidates from variable or anomalous radial velocities, or unusually high rotational velocities. Many SALT survey objects have also been observed by the Transiting Exoplanet Survey Satellite (TESS). TESS light curves provide orbital periods and can also give clues about the nature of binary systems by distinguishing ellipsoidal variations from reflection effects. We present a summary of the candidate binary fraction within the SALT survey, as well as a breakdown of the identified candidates by spectral and helium class.
{"title":"The close binary fraction of He-rich hot subdwarfs from SALT and TESS","authors":"E. J. SNOWDON, C. S. JEFFERY, S. SCHLAGENHAUF","doi":"10.25518/0037-9565.11278","DOIUrl":"https://doi.org/10.25518/0037-9565.11278","url":null,"abstract":"The Southern African Large Telescope (SALT) survey of He-rich hot subdwarfs has identi-fied several binary candidates from variable or anomalous radial velocities, or unusually high rotational velocities. Many SALT survey objects have also been observed by the Transiting Exoplanet Survey Satellite (TESS). TESS light curves provide orbital periods and can also give clues about the nature of binary systems by distinguishing ellipsoidal variations from reflection effects. We present a summary of the candidate binary fraction within the SALT survey, as well as a breakdown of the identified candidates by spectral and helium class.","PeriodicalId":35838,"journal":{"name":"Bulletin de la Societe Royale des Sciences de Liege","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2023-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135053188","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2023-01-01DOI: 10.25518/0037-9565.11186
Valerie VAN GROOTEL, Ingrid Pelisoli
Foreword The 10th Meeting on Hot Subdwarfs and Related Objects (tagged as "sdOB10") was held at University of Liège, Belgium, in June 13-17, 2022 (www.sdOB10.uliege.be). The meeting gathered 75 participants from all around the world, with 60 people on site and 15 participants online, via the live retransmission. This gathering celebrated the 10th edition of this series of meetings initiated in 2003 in Keele (UK) and devoted to hot subdwarf stars. These little blue objects represent an advanced stage of stellar evolution, at least after the first red giant branch (the details of their formation from single, binary and merger channels are still discussed nowa-days), and have attracted a vibrant community of researchers in the last decades for addressing the series of challenges these stars represent. These challenges were reflected in the six sessions organised at the sdOB10 meeting: (1) Atmospheric studies of hot subdwarfs; (2) Populations of hot subdwarfs (both from large surveys and synthesis studies); (3) Pulsations in hot subdwarfs; (4) Hot subdwarfs as laboratories for stellar physics; (5) Origin and evolution of hot subdwarfs; and (6) Massive, compact, low-mass and substellar companions to hot subdwarfs. 58 talks were presented during these six sessions, including 14 flash-talks of 5 minutes showcasing 14 posters that were uploaded on the conference repository. In addition, 3 general discussions were organised along the meeting, fostering collaborations and opening paths
{"title":"10th Meeting on Hot Subdwarfs and Related Objects (tagged as \"sdOB10\") held at University of Liège, Belgium, in June 13-17, 2022","authors":"Valerie VAN GROOTEL, Ingrid Pelisoli","doi":"10.25518/0037-9565.11186","DOIUrl":"https://doi.org/10.25518/0037-9565.11186","url":null,"abstract":"Foreword The 10th Meeting on Hot Subdwarfs and Related Objects (tagged as \"sdOB10\") was held at University of Liège, Belgium, in June 13-17, 2022 (www.sdOB10.uliege.be). The meeting gathered 75 participants from all around the world, with 60 people on site and 15 participants online, via the live retransmission. This gathering celebrated the 10th edition of this series of meetings initiated in 2003 in Keele (UK) and devoted to hot subdwarf stars. These little blue objects represent an advanced stage of stellar evolution, at least after the first red giant branch (the details of their formation from single, binary and merger channels are still discussed nowa-days), and have attracted a vibrant community of researchers in the last decades for addressing the series of challenges these stars represent. These challenges were reflected in the six sessions organised at the sdOB10 meeting: (1) Atmospheric studies of hot subdwarfs; (2) Populations of hot subdwarfs (both from large surveys and synthesis studies); (3) Pulsations in hot subdwarfs; (4) Hot subdwarfs as laboratories for stellar physics; (5) Origin and evolution of hot subdwarfs; and (6) Massive, compact, low-mass and substellar companions to hot subdwarfs. 58 talks were presented during these six sessions, including 14 flash-talks of 5 minutes showcasing 14 posters that were uploaded on the conference repository. In addition, 3 general discussions were organised along the meeting, fostering collaborations and opening paths","PeriodicalId":35838,"journal":{"name":"Bulletin de la Societe Royale des Sciences de Liege","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2023-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135053154","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2023-01-01DOI: 10.25518/0037-9565.11238
Thayse A. PACHECO, Ronaldo S. LEVENHAGEN, Marcos P. DIAZ, Paula R. T. COELHO
We present an update of the grid of detailed atmosphere models and homogeneous synthetic spectra for hot, high-gravity subdwarf stars. High-resolution spectra and synthetic photometry were calculated in the wavelength range 1,000 Å – 10,000 Å using Non-LTE extensively line-blanketed atmosphere structures.
我们提出了热的、高重力的亚矮星的详细大气模型网格和均匀合成光谱的更新。在波长范围为1,000 Å - 10,000 Å的高分辨率光谱和合成光度计算使用非lte广泛线覆盖的大气结构。
{"title":"A grid of Non-LTE line-blanketed atmosphere structures and synthetic spectra for subdwarfs","authors":"Thayse A. PACHECO, Ronaldo S. LEVENHAGEN, Marcos P. DIAZ, Paula R. T. COELHO","doi":"10.25518/0037-9565.11238","DOIUrl":"https://doi.org/10.25518/0037-9565.11238","url":null,"abstract":"We present an update of the grid of detailed atmosphere models and homogeneous synthetic spectra for hot, high-gravity subdwarf stars. High-resolution spectra and synthetic photometry were calculated in the wavelength range 1,000 Å – 10,000 Å using Non-LTE extensively line-blanketed atmosphere structures.","PeriodicalId":35838,"journal":{"name":"Bulletin de la Societe Royale des Sciences de Liege","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2023-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135053178","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2023-01-01DOI: 10.25518/0037-9565.11283
Eric STRINGER, Thomas KUPFER, Matti DORSCH
We present follow-up studies of three ultracompact hot subdwarf binaries. Using data from the Zwicky Transient Facility, we find orbital periods of 33.6, 37.3, and 36.9 minutes for ZTF 1946+3203, ZTF 0640+1738, and ZTF 0643+0318 respectively. The light curves show el-lipsoidal variability of the hot subdwarf star with potential eclipses of an accretion disc. Phase-resolved spectroscopic observations with Keck were used to measure a radial velocity curve and atmospheric parameters of the hot subdwarf stars. ZTF J0643 shows evidence of accretion disc emission lines in the average spectrum. Combining light curve and spectroscopic fits will allow us to measure precise system properties such as masses, to determine the evolutionary history and future evolution of the system.
{"title":"Detailed follow up studies of three ultracompact sdB binaries","authors":"Eric STRINGER, Thomas KUPFER, Matti DORSCH","doi":"10.25518/0037-9565.11283","DOIUrl":"https://doi.org/10.25518/0037-9565.11283","url":null,"abstract":"We present follow-up studies of three ultracompact hot subdwarf binaries. Using data from the Zwicky Transient Facility, we find orbital periods of 33.6, 37.3, and 36.9 minutes for ZTF 1946+3203, ZTF 0640+1738, and ZTF 0643+0318 respectively. The light curves show el-lipsoidal variability of the hot subdwarf star with potential eclipses of an accretion disc. Phase-resolved spectroscopic observations with Keck were used to measure a radial velocity curve and atmospheric parameters of the hot subdwarf stars. ZTF J0643 shows evidence of accretion disc emission lines in the average spectrum. Combining light curve and spectroscopic fits will allow us to measure precise system properties such as masses, to determine the evolutionary history and future evolution of the system.","PeriodicalId":35838,"journal":{"name":"Bulletin de la Societe Royale des Sciences de Liege","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2023-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135052347","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2023-01-01DOI: 10.25518/0037-9565.11251
Francisco J. POZUELOS, Valerie VAN GROOTEL, Antoine THUILLIER, Martín DÉVORA-PAJARES
The main goal of this project is to investigate star-planet interactions during the Red Giant Branch (RGB) phase. In particular, we focus on what happens to planetary systems once their host stars leave the main sequence and engulf close-in planets, presumably, perturbing the dy-namical architecture of the system. In this context, we wonder if close-in planets may survive this evolutionary phase, evolving towards a new stable configuration, or on the contrary, if these planets are destroyed and the entire system collapses. Whatever the outcome, how will this interaction alter the star and affect its subsequent evolution? Here, we search for observational evidence of transiting planets orbiting hot subdwarfs (sdBs) stars, which are direct post-RGB objects that have lost most of their envelopes. To this end, we analyze light curves from the space missions Kepler/K2, TESS, and CHEOPS to search for shallow periodic transits of close-in, previously engulfed planets or their remnants, such as the rocky cores of giant gas planets. By determining the occurrence of planets or remnants around sdB stars, we will place strong constraints on the evolution of planetary systems after the RGB phase of their host stars. This summary describes the methods, tools, and strategies used to explore the available photometric data in the search for transiting planets and establish detection limits that allow us to build planet occurrence rates around these stars.
{"title":"The search for transiting planets around hot subdwarfs","authors":"Francisco J. POZUELOS, Valerie VAN GROOTEL, Antoine THUILLIER, Martín DÉVORA-PAJARES","doi":"10.25518/0037-9565.11251","DOIUrl":"https://doi.org/10.25518/0037-9565.11251","url":null,"abstract":"The main goal of this project is to investigate star-planet interactions during the Red Giant Branch (RGB) phase. In particular, we focus on what happens to planetary systems once their host stars leave the main sequence and engulf close-in planets, presumably, perturbing the dy-namical architecture of the system. In this context, we wonder if close-in planets may survive this evolutionary phase, evolving towards a new stable configuration, or on the contrary, if these planets are destroyed and the entire system collapses. Whatever the outcome, how will this interaction alter the star and affect its subsequent evolution? Here, we search for observational evidence of transiting planets orbiting hot subdwarfs (sdBs) stars, which are direct post-RGB objects that have lost most of their envelopes. To this end, we analyze light curves from the space missions Kepler/K2, TESS, and CHEOPS to search for shallow periodic transits of close-in, previously engulfed planets or their remnants, such as the rocky cores of giant gas planets. By determining the occurrence of planets or remnants around sdB stars, we will place strong constraints on the evolution of planetary systems after the RGB phase of their host stars. This summary describes the methods, tools, and strategies used to explore the available photometric data in the search for transiting planets and establish detection limits that allow us to build planet occurrence rates around these stars.","PeriodicalId":35838,"journal":{"name":"Bulletin de la Societe Royale des Sciences de Liege","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2023-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135052658","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2023-01-01DOI: 10.25518/0037-9565.11294
Murat UZUNDAG, Roberto SILVOTTI, Andrzej S. BARAN, Maja VUčKOVIć, Péter NÉMETH, Sumanta K. SAHOO, Mike REED
TIC 033834484 and TIC 309658435 are long-period pulsating subdwarf B stars, which were observed extensively (675 and 621 days, respectively) by the Transiting Exoplanet Sur-vey Satellite (TESS). The high-precision photometric light curve reveals the presence of more than 40 pulsation modes including both stars. All the oscillation frequencies that we found are associated with gravity (g)-mode pulsations, with frequencies spanning from ∼80 µHz (2 500 s) to ∼400 µHz (12 000 s). We utilize the asteroseismic tools including asymptotic period spacings and rotational frequency multiplets in order to identify the pulsational modes. We found dipole (l = 1) mode sequences for both targets and calculate the mean period spacing of dipole modes (ΔPl=1), which allows us to identify the modes. Frequency multiplets provide a rotation period of ∼64 d for TIC 033834484. From follow-up ground-based spectroscopy, we find that TIC 033834484 has an effective temperature of 24 210 K (140), a surface gravity of log g/cms-2 = 5.28 (03) and TIC 309658435 has an effective temperature of 25 910 K (150), a surface gravity of log g/cms-2 = 5.48 (03).
{"title":"Asteroseismology of hot subdwarf B stars observed with TESS: discovery of two new gravity mode pulsating stars","authors":"Murat UZUNDAG, Roberto SILVOTTI, Andrzej S. BARAN, Maja VUčKOVIć, Péter NÉMETH, Sumanta K. SAHOO, Mike REED","doi":"10.25518/0037-9565.11294","DOIUrl":"https://doi.org/10.25518/0037-9565.11294","url":null,"abstract":"TIC 033834484 and TIC 309658435 are long-period pulsating subdwarf B stars, which were observed extensively (675 and 621 days, respectively) by the Transiting Exoplanet Sur-vey Satellite (TESS). The high-precision photometric light curve reveals the presence of more than 40 pulsation modes including both stars. All the oscillation frequencies that we found are associated with gravity (g)-mode pulsations, with frequencies spanning from ∼80 µHz (2 500 s) to ∼400 µHz (12 000 s). We utilize the asteroseismic tools including asymptotic period spacings and rotational frequency multiplets in order to identify the pulsational modes. We found dipole (l = 1) mode sequences for both targets and calculate the mean period spacing of dipole modes (ΔPl=1), which allows us to identify the modes. Frequency multiplets provide a rotation period of ∼64 d for TIC 033834484. From follow-up ground-based spectroscopy, we find that TIC 033834484 has an effective temperature of 24 210 K (140), a surface gravity of log g/cms-2 = 5.28 (03) and TIC 309658435 has an effective temperature of 25 910 K (150), a surface gravity of log g/cms-2 = 5.48 (03).","PeriodicalId":35838,"journal":{"name":"Bulletin de la Societe Royale des Sciences de Liege","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2023-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135053204","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2023-01-01DOI: 10.25518/0037-9565.11449
Michel Blondieau, Stéphane Puccio, Frédéric Hatert, Martin Depret, Fabrice Dal Bo
Les deux collines du Thier del Preu et du Thier du Mont, situées au nord du village de Grand-Sart (Lierneux), abritent un gisement de coticule dont la minéralogie est peu connue. Un échantillonnage exhaustif durant plus d'une vingtaine d'années a permis d'y recenser une quarantaine d'espèces minérales, dont certaines très rares comme l’éosphorite et la kolbeckite. La minéralogie de cette zone s'avère donc tout aussi intéressante que celle du premier gisement de coticule où se trouvent les localités minéralogiques bien connues de Bihain, Regné et Ottré. Cet article met également en évidence la complexité et la diversité minéralogique de chacun des trois membres de la Formation d'Ottré à Grand-Sart, et une comparaison est faite avec celle observée dans les autres localités proches où affleurent les mêmes formations géologiques.
Thier del Preu和Thier du Mont两座山位于Grand-Sart (Lierneux)村的北部，是coticule矿床的所在地，其矿物学鲜为人知。经过20多年的详尽取样，确定了大约40种矿物，包括一些非常罕见的矿物，如钕石和科尔贝克石。因此，该地区的矿物学与第一个coticule矿床的矿物学一样有趣，那里有著名的Bihain、regne和ottre矿床。本文还强调了Grand-Sart ottre组三个成员的复杂性和矿物学多样性，并将其与附近其他地方观察到的相同地质构造进行了比较。
{"title":"Minéralogie de la Formation d'Ottré au Thier del Preu et au Thier du Mont à Grand-Sart (Lierneux, Belgique), et comparaison avec les autres gisements régionaux","authors":"Michel Blondieau, Stéphane Puccio, Frédéric Hatert, Martin Depret, Fabrice Dal Bo","doi":"10.25518/0037-9565.11449","DOIUrl":"https://doi.org/10.25518/0037-9565.11449","url":null,"abstract":"Les deux collines du Thier del Preu et du Thier du Mont, situées au nord du village de Grand-Sart (Lierneux), abritent un gisement de coticule dont la minéralogie est peu connue. Un échantillonnage exhaustif durant plus d'une vingtaine d'années a permis d'y recenser une quarantaine d'espèces minérales, dont certaines très rares comme l’éosphorite et la kolbeckite. La minéralogie de cette zone s'avère donc tout aussi intéressante que celle du premier gisement de coticule où se trouvent les localités minéralogiques bien connues de Bihain, Regné et Ottré. Cet article met également en évidence la complexité et la diversité minéralogique de chacun des trois membres de la Formation d'Ottré à Grand-Sart, et une comparaison est faite avec celle observée dans les autres localités proches où affleurent les mêmes formations géologiques.","PeriodicalId":35838,"journal":{"name":"Bulletin de la Societe Royale des Sciences de Liege","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2023-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135261889","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Ticks are hematophagous arthropods and obligate ectoparasites with a cosmopolitan distribution. They are of great medical and veterinary importance. Studying the composition of the tick fauna is a crucial step in establishing vector control programs. In this context, an inventory of hard ticks infesting small ruminants in the Tizi-Ouzou area was carried out over a one-year period, from December 2020 to November 2021. Using the direct collection technique on the host animal, a total of 663 animals examined, 170 were infested and a total of 1318 adult tick’s specimens were collected in four sampling sites. The result shows a tick diversity comprising six different species. The most abundant species was Rhipicephalus bursa (68.66%), followed by Rhipicephalus sanguineus (29.74%) and Ixodes ricinus (1.36%). Other species were less abundant, each representing only 0,08% of the total abundance. The highest specific richness was recorded in the Ain El Hammam site located at high altitude. A positive correlation was observed between the farms’ altitude and the tick diversity. The result of FCA analysis showed that distribution of ticks is related to altitude and habitat of tick’s species.
蜱是一种世界性分布的食血节肢动物和专性体外寄生虫。它们具有重要的医学和兽医意义。研究蜱虫区系的组成是制定病媒控制规划的关键步骤。在此背景下，从2020年12月至2021年11月，对Tizi-Ouzou地区侵害小型反刍动物的硬蜱进行了为期一年的清查。采用宿主动物直接采集法，在4个采样点共检测动物663只，侵染动物170只，采集成蜱标本1318只。结果显示，蜱虫的多样性包括六种不同的物种。种类最多的是法氏根头蜱(68.66%)，其次是血根头蜱(29.74%)和蓖麻伊蚊(1.36%)。其他种类较少，每一种只占总丰度的0.08%。高海拔地区的Ain El Hammam遗址比丰富度最高。农场海拔高度与蜱虫多样性呈正相关。FCA分析结果表明，蜱的分布与海拔高度和生境有关。
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