54 research outputs found
Planetary formation seen with ALMA : gas and dust properties in protoplanetary disks around young low-mass stars
No full textCette thèse porte sur l’étude des propriétés du gaz et de la poussière dans le disque protoplanétaire entourant l’étoile jeune triple de faible masse (∼ 1.2 M⊙) GG Tau A. Comprendre les propriétés dynamiques, physiques et chimiques des systèmes stellaires multiples est nécessaire pour comprendre comment une planète peut se former et survivre dans ces environnements complexes. Les interactions gravitationnelles, dues à la multiplicité stellaire, créent une cavité centrale dans le disque protoplanétaire, la matière (gaz et poussières) se répartissant alors près des étoiles (disques internes) et en un anneau situé au delà de la cavité. Dans la cavité, le gaz et la poussière transitent sous la forme de filaments ("streamers") qui nourrissent les disques internes permettant aux étoiles centrales (puis aux planètes) de se former. Ce travail consiste en l’analyse de l’émission de CO (12CO, 13CO et C18O) et de CS observées dans le domaine millimétrique/sub-millimétrique ainsi que des cartes de l’émission thermique de la poussière. L’ émission de 12CO fournit des informations sur la couche moléculaire proche de l’atmosphère du disque, 13CO et C18O, qui sont moins abondants, apportent des informations sur des couches plus profondes, tandis que l’émission de CS devrait être plus proche du plan médian. L’ émission de la poussière permet de caractériser les propriétés du disque de poussières autour de ce même plan.Après avoir introduit le sujet, je présente l’analyse de la morphologie du disque de poussières et de gaz et de sa cinématique qui est dérivée de l’émission de CO.Je présente également un modèle de transfert radiatif de la partie dense du disque (l’anneau) réalisé à partir des donnés CO et CS. La soustraction de ce modèle d’anneau aux données originales révèle l’émission ténue du gaz moléculaire située dans la cavité. Ainsi, je suis en mesure d’évaluer les propriétés des filaments de gaz à l’intérieur de cette cavité, telles que: la dynamique et les conditions d’excitation du gaz en- tourant les trois étoiles et la quantité de masse dans la cavité. Le disque externe est en rotation keplerienne jusqu’au bord interne de l’anneau dense à ∼ 160au. Le disque est relativement froid avec une température pour le gaz (CO) de 25 K et une température pour les poussières de 14 K à 200 ua environ des étoiles centrales. Les températures du gaz et de la poussière chutent très rapidement (∝ r−1). La dynamique du gaz à l’intérieur de la cavité est dominée par la rotation Keplerienne,la contribution de mouvement de chute ("infall") étant évaluée à ∼ 10 − 15% de la vitesse Keplerienne. La température du gaz est de l’ordre de 40 to 80 K. La densité de colonne pour CO et la densité de H2 le long des “streamers”, proches des étoiles (environ 0.3′′ − 0.5′′), sont de l’ordre de quelques 1017 cm−2 et 107 cm−3, respective- ment. La masse totale de gaz à l’intérieur de la cavité est de ∼ 1.6 × 10−4 M⊙ et le taux d’accrétion est de l’ordre de 6.4 × 10−8 M⊙ yr−1. Ces résultats permettent de dresser la première vision un tant soit peu complète de la physique d’un système multiple jeune capable de former des planètes.La chimie dans l’anneau est aussi discutée. Je présente ainsi la première détec- tion de H2S dans un disque protoplanétaire et les détections de DCO+, HCO+ et H13CO+ dans le disque de GG Tau A. Mon analyse des observations et la modélisa- tion chimique associée suggèrent que notre compréhension de la chimie du Soufre est encore incomplète . Dans GG Tau A, la détection de H2S a probablement été possible car le disque est plus massif (facteur ∼ 3 − 5) que les autres disques sur lesquels H2S a été recherché. Une telle masse rend le système adapté à la détection de molécules rares, faisant de lui un bon candidat pour étudier la chimie dans les disques protoplanétaires.This thesis presents the analysis of the gas and dust properties of the protoplanetary disk surrounding the young low-mass (∼ 1.2 M⊙) triple star GG Tau A. Studying such young multiple stars is mandatory to understand how planets can form and survive in such systems shaped by gravitational disturbances. Gravitational interactions linked to the stellar multiplicity create a large cavity around the stars, the matter (gas and dust) being either orbiting around the stars (inner disks) or beyond the cavity (outer disk). In between, the matter is streaming from the outer disk onto the inner disks to feed up the central stars (and possible planets).This work makes use of millimeter/sub-millimeter observations of rotational lines of CO (12CO, 13CO and C18O) together with dust continuum maps. While the 12CO emission gives information on the molecular layer close to the disk atmosphere, its less abundant isotopologues (13CO and C18O) bring information much deeper in the molecular layer. The dust mm emission samples the dust disk around the mid-plane.After introducing the subject, I present the analysis of the morphology of the dust and gas disk. The disk kinematics is derived from the CO analysis. I also present a radiative transfer model of the ring in CO. The subtraction of this model from the original data reveals the weak emission of the molecular gas lying inside the cavity. Thus, I am able to evaluate the properties of the gas inside the cavity, such as the gas dynamics and excitation conditions and the amount of mass in the cavity. The outer disk is in Keplerian rotation until the inner edge of the dense ring at ∼ 160 au. The disk is relatively cold with a CO gas temperature of 25 K and a dust temperature of ∼14 K at 200 au from the central stars. Both CO gas and dust temperatures drop very fast (∝ r−1). The gas dynamics inside the cavity is dominated by Keplerian rotation motion. The contribution of infall motion is evaluated at ∼ 10 − 15% of the Keplerian velocity. The gas temperature inside the cav- ity is of the order of 40 − 80 K. The CO column density and H2 density along the “streamers”, which are close to the binary components (around 0.3′′ − 0.5′′) are of the order of a few 1017 cm−2 and 107 cm−3, respectively. The total mass of gas inside the cavity is ∼ 1.6 × 10−4 M⊙ and the accretion rate is estimated at the level of 6.4 × 10−8 M⊙ yr−1. These new results provide the first quantitative global picture of the physical properties of a protoplanetary disk orbiting around a young low-mass multiple star able to create planets.I also discuss some chemical properties of the GG Tau A disk. I report the first detection of H2S in a protoplanetary disk, and the detections of DCO+, HCO+ and H13CO+ in the disk of GG Tau A. Our analysis of the observations and its chemical modeling suggest that our understanding of the S chemistry is still incomplete. In GG Tau A, the detection of H2S has been likely possible because the disk is more massive (a factor ∼ 3 − 5) than other disks where H2S was searched. Such a large disk mass makes the system suitable to detect rare molecules and to study cold- chemistry in protoplanetary disks
Planetary formation seen with ALMA : gas and dust properties in protoplanetary disks around young low-mass stars
No full textCette thèse porte sur l’étude des propriétés du gaz et de la poussière dans le disque protoplanétaire entourant l’étoile jeune triple de faible masse (∼ 1.2 M⊙) GG Tau A. Comprendre les propriétés dynamiques, physiques et chimiques des systèmes stellaires multiples est nécessaire pour comprendre comment une planète peut se former et survivre dans ces environnements complexes. Les interactions gravitationnelles, dues à la multiplicité stellaire, créent une cavité centrale dans le disque protoplanétaire, la matière (gaz et poussières) se répartissant alors près des étoiles (disques internes) et en un anneau situé au delà de la cavité. Dans la cavité, le gaz et la poussière transitent sous la forme de filaments ("streamers") qui nourrissent les disques internes permettant aux étoiles centrales (puis aux planètes) de se former. Ce travail consiste en l’analyse de l’émission de CO (12CO, 13CO et C18O) et de CS observées dans le domaine millimétrique/sub-millimétrique ainsi que des cartes de l’émission thermique de la poussière. L’ émission de 12CO fournit des informations sur la couche moléculaire proche de l’atmosphère du disque, 13CO et C18O, qui sont moins abondants, apportent des informations sur des couches plus profondes, tandis que l’émission de CS devrait être plus proche du plan médian. L’ émission de la poussière permet de caractériser les propriétés du disque de poussières autour de ce même plan.Après avoir introduit le sujet, je présente l’analyse de la morphologie du disque de poussières et de gaz et de sa cinématique qui est dérivée de l’émission de CO.Je présente également un modèle de transfert radiatif de la partie dense du disque (l’anneau) réalisé à partir des donnés CO et CS. La soustraction de ce modèle d’anneau aux données originales révèle l’émission ténue du gaz moléculaire située dans la cavité. Ainsi, je suis en mesure d’évaluer les propriétés des filaments de gaz à l’intérieur de cette cavité, telles que: la dynamique et les conditions d’excitation du gaz en- tourant les trois étoiles et la quantité de masse dans la cavité. Le disque externe est en rotation keplerienne jusqu’au bord interne de l’anneau dense à ∼ 160au. Le disque est relativement froid avec une température pour le gaz (CO) de 25 K et une température pour les poussières de 14 K à 200 ua environ des étoiles centrales. Les températures du gaz et de la poussière chutent très rapidement (∝ r−1). La dynamique du gaz à l’intérieur de la cavité est dominée par la rotation Keplerienne,la contribution de mouvement de chute ("infall") étant évaluée à ∼ 10 − 15% de la vitesse Keplerienne. La température du gaz est de l’ordre de 40 to 80 K. La densité de colonne pour CO et la densité de H2 le long des “streamers”, proches des étoiles (environ 0.3′′ − 0.5′′), sont de l’ordre de quelques 1017 cm−2 et 107 cm−3, respective- ment. La masse totale de gaz à l’intérieur de la cavité est de ∼ 1.6 × 10−4 M⊙ et le taux d’accrétion est de l’ordre de 6.4 × 10−8 M⊙ yr−1. Ces résultats permettent de dresser la première vision un tant soit peu complète de la physique d’un système multiple jeune capable de former des planètes.La chimie dans l’anneau est aussi discutée. Je présente ainsi la première détec- tion de H2S dans un disque protoplanétaire et les détections de DCO+, HCO+ et H13CO+ dans le disque de GG Tau A. Mon analyse des observations et la modélisa- tion chimique associée suggèrent que notre compréhension de la chimie du Soufre est encore incomplète . Dans GG Tau A, la détection de H2S a probablement été possible car le disque est plus massif (facteur ∼ 3 − 5) que les autres disques sur lesquels H2S a été recherché. Une telle masse rend le système adapté à la détection de molécules rares, faisant de lui un bon candidat pour étudier la chimie dans les disques protoplanétaires.This thesis presents the analysis of the gas and dust properties of the protoplanetary disk surrounding the young low-mass (∼ 1.2 M⊙) triple star GG Tau A. Studying such young multiple stars is mandatory to understand how planets can form and survive in such systems shaped by gravitational disturbances. Gravitational interactions linked to the stellar multiplicity create a large cavity around the stars, the matter (gas and dust) being either orbiting around the stars (inner disks) or beyond the cavity (outer disk). In between, the matter is streaming from the outer disk onto the inner disks to feed up the central stars (and possible planets).This work makes use of millimeter/sub-millimeter observations of rotational lines of CO (12CO, 13CO and C18O) together with dust continuum maps. While the 12CO emission gives information on the molecular layer close to the disk atmosphere, its less abundant isotopologues (13CO and C18O) bring information much deeper in the molecular layer. The dust mm emission samples the dust disk around the mid-plane.After introducing the subject, I present the analysis of the morphology of the dust and gas disk. The disk kinematics is derived from the CO analysis. I also present a radiative transfer model of the ring in CO. The subtraction of this model from the original data reveals the weak emission of the molecular gas lying inside the cavity. Thus, I am able to evaluate the properties of the gas inside the cavity, such as the gas dynamics and excitation conditions and the amount of mass in the cavity. The outer disk is in Keplerian rotation until the inner edge of the dense ring at ∼ 160 au. The disk is relatively cold with a CO gas temperature of 25 K and a dust temperature of ∼14 K at 200 au from the central stars. Both CO gas and dust temperatures drop very fast (∝ r−1). The gas dynamics inside the cavity is dominated by Keplerian rotation motion. The contribution of infall motion is evaluated at ∼ 10 − 15% of the Keplerian velocity. The gas temperature inside the cav- ity is of the order of 40 − 80 K. The CO column density and H2 density along the “streamers”, which are close to the binary components (around 0.3′′ − 0.5′′) are of the order of a few 1017 cm−2 and 107 cm−3, respectively. The total mass of gas inside the cavity is ∼ 1.6 × 10−4 M⊙ and the accretion rate is estimated at the level of 6.4 × 10−8 M⊙ yr−1. These new results provide the first quantitative global picture of the physical properties of a protoplanetary disk orbiting around a young low-mass multiple star able to create planets.I also discuss some chemical properties of the GG Tau A disk. I report the first detection of H2S in a protoplanetary disk, and the detections of DCO+, HCO+ and H13CO+ in the disk of GG Tau A. Our analysis of the observations and its chemical modeling suggest that our understanding of the S chemistry is still incomplete. In GG Tau A, the detection of H2S has been likely possible because the disk is more massive (a factor ∼ 3 − 5) than other disks where H2S was searched. Such a large disk mass makes the system suitable to detect rare molecules and to study cold- chemistry in protoplanetary disks.Chủ đề nghiên cứu của luận án là về tính chất của khí và bụi trên đĩa tiền hành tinhquanh một hệ đa sao có khối lượng ∼1.2 Msun, GG Tau A. Nghiên cứu các hệ đa saotrẻ là cần thiết để hiểu về sự hình thành và tồn tại của hệ hành tinh trong môi trườngnhiễu loạn hấp dẫn. Tương tác hấp dẫn của hệ đa sao tạo nên một khoang rỗng lớnxung quanh các sao thành phần, vật chất (khí và bụi) của hệ có thể quay quanh từngsao đơn ("đĩa trong") và bên ngoài khoang rỗng, xung quanh cả hệ sao ("đĩa ngoài").Ở giữa hai phần này của hệ, vật chất được truyền từ đĩa ngoài vào đĩa trong để nuôidưỡng các sao ở trung tâm (hoặc có thể cả hành tinh).Nghiên cứu của luận án sử dụng các quan sát thiên văn vô tuyến ở bướcsóng millimet/dưới-millimet phát ra bởi các phân tử CO (12CO, 13CO và C18O) và bụi.Phát xạ từ 12CO cung cấp thông tin về lớp phân tử gần với khí quyển của đĩa, cácđồng phân kém phổ biến hơn (13CO và C18O) cung cấp thông tin nằm sâu hơn tronglớp phân tử của đĩa. Phát xạ mm của bụi giúp nghiên cứu các tính chất trên mặtphẳng giữa của đĩa.Sau khi giới thiệu về chủ đề và đối tượng nghiên cứu, tôi trình bày về hình tháivà động học của đĩa khí và bụi của hệ sao. Tôi cũng trình bày mô hình truyền bức xạcủa đĩa ngoài sử dụng các đồng phân của CO. Đĩa ngoài của hệ tuân theo chuyểnđộng Kepler cho đến gần khoang rỗng, ∼160 au từ tâm sao, và tương đối lạnh. Nhiệtđộ khí CO và bụi lần lượt là 25K và 14K tại khoảng cách 200au, và giảm nhanh khikhoảng cách tới tâm tăng, T ∝ r−1. Việc trừ mô hình đĩa ngoài từ số liệu ban đầu biểulộ rõ ràng hơn phát xạ yếu của các phân tử khí trong khoang rỗng. Do đó, động họcvà điều kiện phát xạ của khí trong khoang rỗng có thể được đánh giá. Các phân tửkhí bên trong khoang rỗng bị chi phối bởi chuyển động quay, với sự đóng góp nhỏcủa chuyển động rơi được đánh giá vào cỡ 10–15% chuyển động Kepler. Nhiệt độkhí bên trong khoang rỗng trong khoảng 40–80 K, mật độ dài của khí CO và mật độkhối của H2 lần lượt là 1017cm−2 và 107cm−3. Tổng khối lượng khí trong khoang rỗnglà ∼1.6×10−4 Msun, tốc độ truyền vật chất từ đĩa ngoài vào đĩa trong được tính vàokhoảng ∼ 6.4×10−8 Msun yr−1. Các kết quả nghiên cứu này góp phần cung cấp mộtbức tranh tổng quát định lượng đầu tiên về tính chất vật lý của đĩa tiền hành tinhquay xung quanh một hệ đa sao trẻ có khối lượng thấp, nơi có khả năng hình thànhhành tinh.Một vài tính chất hóa học của đĩa tiền hành tinh GG Tau A cũng được nghiêncứu trong luận án này. Tôi trình bày về sự phát hiện lần đầu tiên H2S trong đĩa tiềnhành tinh, cũng như sự phát hiện lần đầu tiên DCO+, HCO+ và H13CO+ trong đĩa GGTau A. Kết quả phân tích số liệu thực nghiệm và mô hình hóa học cho thấy sự hiểubiết của chúng ta về hóa học các phân tử có chứa sulfur trong đĩa là chưa hoànthiện. Trong đĩa tiền hành tinh GG Tau A, khả năng phát hiện được phân tử hiếmnhư H2S có thể là nhờ vào khối lượng lớn của đĩa (lớn hơn khoảng 3–5 lần so vớicác đĩa tiền hành tinh nơi H2S đã từng được tìm kiếm). GG Tau A với đĩa tiền hànhtinh có khối lượng lớn là thích hợp để tìm kiếm các phân tử hiếm và nghiên cứu vềthành phần hóa học của đĩa có nhiệt độ thấp
A Self-Reflexive Verista. Metareference and Autofiction in Luigi Capuana’s Narrative
No full textWith a Preface by Edwige Comoy Fusaro, this volume is one of few monographs on Italian post-Risorgimento author Luigi Capuana, and the first one written in English in more than forty years. Narratology and critical theory are combined with more ‘traditional’, historical-philological criticism to offer a radical rereading of the author’s narrative.
Central to this study is the seemingly counter-intuitive notion of artistic self-reflexivity, which represents an innovative take on an author like Capuana, who has long been ‘canonised’ as a verista.With a Preface by Edwige Comoy Fusaro, this volume is one of few monographs on Italian post-Risorgimento author Luigi Capuana, and the first one written in English in more than forty years. Narratology and critical theory are combined with more ‘traditional’, historical-philological criticism to offer a radical rereading of the author’s narrative.
Central to this study is the seemingly counter-intuitive notion of artistic self-reflexivity, which represents an innovative take on an author like Capuana, who has long been ‘canonised’ as a verista
Metareference and Autofiction in Luigi Capuana’s Narrative
No full textWith a Preface by Edwige Comoy Fusaro, this volume is one of few monographs on Italian post-Risorgimento author Luigi Capuana, and the first one written in English in more than forty years. Narratology and critical theory are combined with more ‘traditional’, historical-philological criticism to offer a radical rereading of the author’s narrative. Central to this study is the seemingly counter-intuitive notion of artistic self-reflexivity, which represents an innovative take on an author like Capuana, who has long been ‘canonised’ as a verista
Expressive Arts Therapy and Oncology Care Teams
No full textThis literature review offers an overview of the mental health of oncology care team members, medical professionals as well as oncology floor hospital staff, and the therapeutic benefits of expressive therapies on that specific population. Working on an oncology floor means interacting with patients and their loved ones at a time of utmost suffering, uncertainty, and possible death. This environment presents risks of burnout, compassion fatigue, and a sense of isolation for the medical and non-medical professionals working with cancer patients. The results of qualitative, quantitative, and art-based studies conducted pre-and post-Covid-19 pandemic show multi-faceted and multi-layered positive impacts of expressive-arts-therapy interventions on the care team and staff members and on that milieu overall. Based on the conclusions of the studies selected for this review, the author presents three types of expressive arts interventions with mindful self-care, grief and loss processing, and vicarious resilience as goals. The author recorded their thesis research and writing process through mixed-media art-journaling after each work session
La dynamique d\u27un engagement « poélitique » : le cas du théâtre de Maryse Condé
No full textMaryse Condé\u27s plays reveal both a scriptural and thematic dynamism. This movement manifests a commitment that renews itself through the dramatization of varied sociopolitical current events. The first plays of the Guadeloupean showcase slavery, colonization and Independence. The problematic of the future of Black peoples flowing from them resounds differently in her recent works. Maryse Condé complexifies it indeed and updates it constantly. This makes her an unconventional author, for her writing takes roots in negritude, partakes in post-negritude and proceeds equally from a dramaturgy of uprootedness
Le mariage et le divorce dans le Code marocain de la famille. Le nouveau droit à l’égalité entre l’homme et la femme
No full textThe author proposes to analyze the most recent reform of Morocco’s family Code. She reminds us that Moroccan family law relies on sacred texts. She gives particular attention to new rulings regarding marriage and divorce, examining the prospects for a family law that is more egalitarian with respect to men and women
Author Correction: Dating the landscape evolution around the Chauvet-Pont d’Arc cave
No full textInternational audienceThe original version of this Article contained an error in the spelling of the author Anne Philippe, which was incorrectly given as Anne Phillippe. The original Article and accompanying Supplementary Information file have been corrected
Fictions souveraines : héritages féministes de la Kahina
No full textL’auteure étudie les multiples réappropriations de l’histoire de la Kahina dans la sphère francophone en procédant à la lecture croisée d’œuvres savantes, publiées par des orientalistes français, et d’ouvrages de fiction, écrits par des femmes. La lecture intertextuelle souligne les mécanismes de formation et de transmission d’un héritage féministe autour de cette souveraine amazighe, dont la légende rapporte qu’elle s’opposa à l’invasion arabe de l’Afrique du Nord au viie siècle. Bien que sa vie et son identité demeurent incertaines, la Kahina s’est prêtée depuis le Moyen Âge « à toutes sortes de récupérations » (Modéran), tour à tour symbole de berbérité, de féminisme, de nationalisme, d’identité juive, ou encore de lutte des classes. Pour les auteures mentionnées dans cet article, s’inscrire dans l’héritage contesté de la Kahina correspond à une « recherche des origines » (Halimi) qui émancipe et relie des femmes d’horizons différents, et traverse la frontière symbolique de la Méditerranée. À travers ces mécanismes d’identification transculturelle, l’auteure de cet article propose de considérer les (ré)appropriations féministes de la Kahina comme des sites potentiels de résistance anti-impériale, retournant l’instrumentalisation qu’en avait faite l’empire français et offrant une réinterprétation de l’histoire à travers la fiction. La Kahina devient figure de proue d’un panthéon féministe transculturel, sans cesse réinventé.The author studies the multiple reappropriations of the Kahina’s story in the Francophone world by bringing together two corpora: the works of French orientalists and the fiction of women writers. The intertextual reading underlines the mechanisms of formation and transmission of a feminist heritage around this Amazigh queen, who opposed the Arab invasion of North Africa in the seventh century. Although her life and identity remain uncertain, the Kahina has lent herself « to all sorts of recuperations » since the Middle Ages (Modéran), in turn a symbol of Berberism, feminism, nationalism, Jewish identity, and class struggle. For the authors discussed in this article, being part of the contested heritage of the Kahina corresponds to a « search for origins » (Halimi) that emancipates and connects women from different backgrounds to cross the symbolic border of the Mediterranean. Through such mechanisms of transcultural identification, the author of this article proposes to consider feminist (re)appropriations of the Kahina as acts of anti-imperial resistance, turning her instrumentalization by the French empire on its head and offering a reinterpretation of history through fiction. The Kahina becomes the figurehead of a transcultural feminist pantheon, constantly reinvented.La autora estudia las múltiples reapropiaciones de la historia de la Kahina en el ámbito francófono mediante una lectura cruzada de obras eruditas, publicadas por orientalistas franceses, y de obras de ficción, escritas por mujeres. La lectura intertextual subraya los mecanismos de formación y de transmisión de una herencia feminista en torno a esta soberana amazig, cuya leyenda cuenta que se opuso a la invasión árabe del norte de África en el siglo VII. Aunque su vida e identidad siguen siendo inciertas, la Kahina se ha prestado desde la Edad Media « a todo tipo de recuperaciones » (Moderan), a su vez símbolo de bereberismo, de feminismo, de nacionalismo, de identidad judía o más de lucha de clases. Para las autoras mencionadas en este artículo, formar parte de la herencia contestada de la Kahina corresponde a una « búsqueda de orígenes » (Halimi) que emancipa y conecta a mujeres de diferentes orígenes, y cruza la frontera simbólica del Mediterráneo. A través de estos mecanismos de identificación transcultural, la autora de este artículo propone considerar las (re)apropiaciones feministas de la Kahina como sitios potenciales de resistencia antiimperialista, revirtiendo la instrumentalización que hizo de ellas el imperio francés y ofreciendo una reinterpretación de la historia a través de la ficción. La Kahina se convierte en la figura destacada de un panteón feminista transcultural, en constante reinvención
Capuana Critico (Di Dossi)
No full textIn his introduction to the collection of Luigi Capuana’s Scritti critici (1972), Ermanno Scuderi claims that the renowned theorist of Verismo was a pioneer in contemporary literary criticism. The aim of the following contribution is to explore this claim, by analysing Capuana’s reviews of Carlo Dossi’s books, published while the author was still alive. Dossi was, and still is, regarded as difficult to read and understand, mainly for linguistic reasons. Although the review of Dossi’s first book by Cletto Arrighi was laudatory, other reviewers were overwhelmingly negative, until an elaborated piece of dossian criticism was released, featuring essays by Luigi Perelli, Giuseppe Antonio Borgese and Gian Pietro Lucini (1910-1911). In an essay devoted to Dossi in Studi sulla letteratura contemporanea, Capuana shows perspicacity and foresight. Therefore, Capuana’s literary criticism proves to be of particular interest for its role in establishing a canon of the late 19th century.
Keywords: critica letteraria, Carlo Dossi, Luigi Capuana, Ottocento italiano
- …
